cataclysmics, symbiotics, novae - astrosurf · aras eruptive stars information letter #40 2018-04 -...

Eruptive stars spectroscopyCataclysmics, Symbiotics, Novae

Eruptive StarsInformation Letter n° 40 #2018-04 20-02-2019

Observations of Oct. - Dec. 2018Contents

Nova

Spectrum of Nova Sct 2017 in nebular phase

Symbiotics

V694 Mon = MWC 560: absorptions have goneThe new symbiotic HaHb 1705-04: declining outburstZ And outburst (declining)

Spectra of a new symbiotic star: Hen 3-1768

Notes

The music of the spheresSteve Shore

“We acknowledge with thanks the variable star observations from the AAVSO International Database contributed by observers worldwide and used in this letter.”Kafka, S., 2015, Observations from the AAVSO International Database, http://www.aavso.org

F. Teyssier, S. Shore, J. Guarro, F. Sims, D. Boyd, J. Foster, P. Somogyi, P. Berardi, U. Sollecchia, S. Charbonnel, T. Bohlsen, F. Campos, G. Martineau, Y. Buchet, K. Graham, C. Boussin, F. Boubault, L. Franco, T. Rodda, V. Marik, C. Buil, T. Kantola, J. Coffin

p. 2

p. 4

p. 40

p. 77

Authors :

ARAS Eruptive Stars Information Letter #40 2018-04 - p. 2

List of galactic novae in 2018

A new spectrum of nova Sct 2017 in nebular phase obtained by James Foster

Spectroscopic observations of novae in 2018-Q4Nova Sct 2017

Abstract

Teyssier, F. , Foster, J. R.

Authors

GCVSName Date Mag A.D. (2000) DE (2000)

15 nova Nor 2018 V0556 Nor PNV J16143400-5330050 2018-10-13.414 10.5 16 14 32.92 -53 30 14.7 10.214 nova Oph 2018c V3664 Oph PNV J17422408-2053088 2018-8 8.960 17 42 24.08 -20 53 08.8 913 nova Sct 2018 V0613 Sct TCP J18292290-1430460 2018-6-29.577 18 29 22.93 -14 30 44.2 10.512 nova Lup 2018 V0408 Lup PNV J15384000-4744500 2018-6-3.431 15 38 43.84 -47 44 41.1 911 nova Per 2018 V0392 Per TCP J04432130+4721280 2018 -4-29.740 04 43 21.37 +47 21 25.8 6.310 nova Sgr 2018 V5857 Sgr PNV J18040967-1803581 2018-4-8.72 11.2 18 04 09.46 -18 03 55.7 10.89 nova CMa 2018 V0435 CMa TCP J07134590-2112330 2018-3-24.496 12 07 13 45.84 -21 12 31.3 10.38 nova Car 2018 V0906 Car ASASSN-18fv 2018-3-20.32 <10.0 10 36 13.71 -59 35 55.1 5.97 nova Oph 2018b V3665 Oph PNV J17140261-2849237 2018-3-10.805 9.4 17 14 2.53 -28 49 23.3 9.46 nova Sco 2018c V1663 Sco ASSASN-18ds 2018-2-24.36 14.3 17 3 47.509 -38 16 57.14 9.85 nova Oph 2018 V3664 Oph PNV J17244011-2421463 2018-2-12.834 12.5 17 24 40.11 -24 21 46.3 12.84 nova Sco 2018b V1662 Sco PNV J16484962-4457032 2018-2-6.863 11.7 16 48 49.68 -44 57 2.9 10.13 nova Cir 2018 FM Cir PNV J13532700-6725110 2018-1-19.708 9.1 13 53 27.59 -67 25 0.9 5.72 nova Sco 2018 V1661 Sco PNV J17180658-3204279 2018-1-17.869 11 17 18 6.37 -32 4 27.7 10.21 nova Mus 2018 V0357 Mus PNV J11261220-6531086 2018-1-14.486 11 26 15.16 -65 31 23.3 6.5

# Coordinates Mag MaxName Discovery

Updated with GCVS namesNovae in 2018: Official Announcement of GCVS NamesKazarovets, E. V.; Samus, N. N.http://www.astronet.ru/db/varstars/msg/1452269

NOVAE

Nova Sct 2017

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Nova Sct 2017 2018-10-14 02:59:00 R = 539 James R. Foster

4000 4500 5000 5500 6000 6500 7000

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Nova Sct 2017 2018-10-14 02:59:00 R = 539 James R. Foster


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142457840 2457960 2458080 2458200 2458320 2458440 2458560

Nova Sct 2017 (V)


Authors:F. Teyssier, D. Boyd, J. Guarro, F. Sims, D. Boyd, J. Foster, P. Somogyi, P. Berardi, U. Sollecchia, S. Charbonnel, T. Bohlsen, F. Campos, G. Martineau, Y. Buchet, K. Graham, C. Boussin, F. Bou-bault, L. Franco, T. Rodda, V. Marik, C. Buil, T. Kantola, J. Coffin

Spectroscopic observations of symbiotic stars in 2018-Q4

ARAS Eruptive Stars Information Letter #40 2018-04

Abstract:

202 spectra of 26 symbiotic stars at resolution from 500 to 15000 were obtained during 2018-Q4.AG Dra has recovered its quiescent state after April 2018 outburst. CH Cyg has been monitoring at a high cadency during its monotonically decline from mag V = 6.4 early august to V = 8.5. More than 700 spectra of CH Cygni are now gathered in the database. First spectrum of the poorly studied EF Aql in the database. Spectra of the new symbiotic Hen 3-1768 detected within the context of the program "suspected symbiotic stars" show strong He II l 4686 and Raman OVI 6830. The new sym-biotic star HbHa 1704-058 observed during its decline show increasing raman OVI band (EW = -3.3) while [OIII] and [Fe VII] remain very weak if present. V694 Mon, at high luminosity (V ~ 9) , presents unusual shape of Balmer and Fe II lines: the common broad absorption is replaced by P Cygni profiles at much lower velocities (maximum of absorption ~ -100 km s-1). The prototypical Z And returns to quiescent state after the outburst which occurred in January 2018.

EG And, V471 Per, BD Cam, StHa 32, UV Aur, V1261 Ori, StHA 55, SU Lyn, BX Mon, V694 Mon, CQ Dra, AG Dra, V443 Her, BF Cyg, CH Cyg, CI Cyg, EF Aql, TCPJ19544251+1722281, PU Vul, ER Del, V1329 Cyg, StHa 190,

Symbiotics: Observing program

SYMBIOTIC


Observing : main targetsName AD (2000) DE (2000)AG Dra 16 1 40.5 +66 48 9.5AG Peg 21 51 1.9 +12 37 29.4AX Per 01 36 22.7 +54 15 2.5BF Cyg 19 23 53.4 +29 40 25.1BX Mon 07 25 24 -03 36 00CH Cyg 19 24 33 +50 14 29.1CI Cyg 19 50 11.8 +35 41 03.2EG And 00 44 37.1 +40 40 45.7R Aqr 23 43 49.4 -15 17 04.2RS Oph 17 50 13.2 -06 42 28.4SU Lyn 06 42 55.1 +55 28 27.2T CrB 15 59 30.1 +25 55 12.6V443 Her 18 22 8.4 +23 27 20V694 Mon 07 25 51.2 -07 44 08Z And 23 33 39.5 +48 49 5.4

Target Request Objective Notes StatusCH Cyg Independently

A. SkopalM. Karovska

Long term monitoring of a com-plex and highly variable object

Ongoing

AG Dra R. Gàlis J. Merc L. Leedjarv

Study of outburst and orbital vari-ability

He II / HbRaman OVI

One spectrum a week until next outburst (Spring 2019)

SU Lyn K. Drozd Study of the orbital variations of a newly discovered symbiotic

One spectrum a week

V694 Mon A. LucyJ. Sokolovski

Detection of active phases Balmer and Fe II lines New season

ARAS Eruptive Stars Information Letter #40 2018-04

Main targets for 2019, Quarter 1V694 Mon in peculiar state: high cadency monitoring is highly recommendedAX Per, BX Mon, SU LynIn the morning sky : T CrB, CI Cygni, AG Dra

Symbiotics in ARAS Data Base Update : 01-02-2019SYMBIOTICS


58 stars4216 spectra

# Name AD (2000) DE (2000) Nb. of spectra First spectrum Last spectrum Days Since Last

1 EG And 0 44 37.1 40 40 45.7 117 12/08/2010 25/01/2019 82 AX Per 1 36 22.7 54 15 2.5 261 04/10/2011 18/01/2019 153 V471 Per 1 58 49.7 52 53 48.4 28 06/08/2013 10/11/2018 844 Omi Cet 2 19 20.7 -2 58 39.5 31 28/11/2015 14/01/2019 195 BD Cam 03 42 9.3 63 13 0.5 42 08/11/2011 25/01/2019 86 StHa 32 04 37 45.6 -01 19 11.8 5 02/03/2018 05/03/2018 3347 UV Aur 05 21 48.8 32 30 43.1 77 24/02/2011 15/01/2019 188 V1261 Ori 05 22 18.6 -8 39 58 16 22/10/2011 02/12/2018 629 StHA 55 05 46 42 6 43 48 7 17/01/2016 24/01/2019 9

10 SU Lyn 06 42 55.1 +55 28 27.2 129 02/05/2016 20/01/2019 1311 ZZ CMi 07 24 13.9 8 53 51.7 54 29/09/2011 13/04/2018 29512 BX Mon 07 25 24 -3 36 0 56 04/04/2011 22/01/2019 1113 V694 Mon 07 25 51.2 -7 44 8 270 03/03/2011 28/01/2019 514 NQ Gem 07 31 54.5 24 30 12.5 67 01/04/2013 03/01/2019 3015 GH Gem 07 4 4.9 12 2 12 7 10/03/2016 15/12/2017 41416 CQ Dra 12 30 06 69 12 04 27 11/06/2015 18/11/2018 7617 TX CVn 12 44 42 36 45 50.6 56 10/04/2011 09/07/2018 20818 RW Hya 13 34 18 - 25 22 48.9 18 28/06/2017 14/07/2018 20319 IV Vir 14 16 34.3 -21 45 50 10 28/02/2015 11/07/2018 20620 T CrB 15 59 30.1 25 55 12.6 269 01/04/2012 23/09/2018 13221 AG Dra 16 01 40.5 66 48 9.5 507 03/04/2013 12/12/2018 5222 AS 210 16 51 20.4 -26 00 26.7 2 14/06/2018 07/07/2018 21023 V503 Her 17 36 46 23 18 18 5 05/06/2013 15/05/2018 26324 RS Oph 17 50 13.2 -6 42 28.4 48 23/03/2011 20/07/2018 19725 V934 Her 17 06 34.5 +23 58 18.5 32 09/08/2013 31/08/2018 15526 RT Ser 17 39 52.0 -11 56 38.8 2 26/06/2012 13/07/2018 20427 AS 245 17 51 00.9 -22 19 35.1 1 15/07/2018 15/07/2018 20228 AS 270 18 05 33.7 -20 20 38 6 01/08/2013 07/07/2018 21029 AS 289 18 12 22.1 -11 40 07 3 26/06/2012 15/06/2018 23230 YY Her 18 14 34.3 20 59 20 27 25/05/2011 26/09/2018 12931 FG Ser 18 15 06.2 0 18 57.6 7 26/06/2012 22/06/2018 22532 StHa 149 18 18 55.9 27 26 12 6 05/08/2013 13/07/2018 20433 V443 Her 18 22 08.4 23 27 20 59 18/05/2011 11/12/2018 5334 FN Sgr 18 53 52.9 -18 59 42 9 10/08/2013 15/07/2018 20235 V919 Sgr 19 03 46 -16 59 53.9 7 10/08/2013 10/12/2018 5436 V1413 Aql 19 03 51.6 16 28 31.7 13 10/08/2013 10/12/2018 5437 V335 Vul 19 23 14 +24 27 39.7 11 14/08/2016 26/07/2018 19138 BF Cyg 19 23 53.4 29 40 25.1 154 01/05/2011 31/10/2018 9439 CH Cyg 19 24 33 50 14 29.1 724 21/04/2011 05/01/2019 2840 HM Sge 19 41 57.1 16 44 39.9 13 20/07/2013 23/09/2018 13241 QW Sge 19 45 49.6 18 36 50 11 14/08/2016 26/07/2018 19143 CI Cyg 19 50 11.8 35 41 3.2 206 25/08/2010 11/12/2018 5344 StHa 169 19 51 28.9 46 23 6 5 12/05/2016 08/07/2018 20945 EF Aql 19 51 51.7 -05 48 16.7 1 11/11/2018 11/11/2018 8346 TCPJ19544251+172228119 54 42.9 +17 22 12.7 59 09/08/2018 31/10/2018 9447 V1016 Cyg 19 57 4.9 39 49 33.9 18 15/04/2015 10/12/2018 5448 RR Tel 20 04 18.5 -55 43 33.2 3 08/09/2017 30/10/2017 46049 PU Vul 20 21 12 21 34 41.9 21 20/07/2013 10/11/2018 8450 LT Del 20 35 57.3 20 11 34 17 28/11/2015 28/09/2018 12751 ER Del 20 42 46.4 8 40 56.4 11 02/09/2011 20/10/2018 10552 V1329 Cyg 20 51 1.1 35 34 51.2 20 08/08/2015 09/01/2019 2453 V407 Cyg 21 2 13 45 46 30 12 14/03/2010 18/04/2010 054 StHa 190 21 41 44.8 2 43 54.4 22 31/08/2011 21/10/2018 10455 AG Peg 21 51 1.9 12 37 29.4 255 06/12/2009 11/12/2018 5356 V627 Cas 22 57 41.2 58 49 14.9 33 06/08/2013 08/01/2019 2557 Z And 23 33 39.5 48 49 5.4 154 30/10/2010 25/01/2019 858 R Aqr 23 43 49.4 -15 17 4.2 178 20/11/2010 13/12/2018 51

Symbiotic like59 SS Lep 06 04 59.1 -16 29 04.0 5 17/02/2018 22/01/2019 11

Symbiotics observed in October-December, 2018 1/2


Id. Observer Date Res. Id. Observer Date Res.AG Dra F. Campos 03/10/2018 3828 7367 919 CH Cyg J. Guarro 01/10/2018 4053 7762 9000AG Dra J. Guarro 12/10/2018 4053 7762 9000 CH Cyg P. Somogyi 05/10/2018 3824 3981 4578AG Dra D. Boyd 18/10/2018 3901 7381 1110 CH Cyg P. Somogyi 06/10/2018 3822 3980 5119AG Dra S. Charbonnel 19/10/2018 4036 7593 11000 CH Cyg P. Somogyi 12/10/2018 3823 3980 4852AG Dra D. Boyd 18/11/2018 3901 7379 1094 CH Cyg U. Sollecchia 12/10/2018 6387 6766 8380AG Dra F. Campos 24/11/2018 6397 7161 4498 CH Cyg J. Guarro 12/10/2018 3980 7762 9000AG Dra D. Boyd 12/12/2018 3901 7380 1107 CH Cyg T. Kantola 14/10/2018 3603 7405 524AG Peg T. Rodda 21/08/2018 3901 7391 611 CH Cyg P. Somogyi 14/10/2018 3821 3978 4516AG Peg J. Guarro 01/10/2018 4059 7753 9000 CH Cyg F. Teyssier 16/10/2018 4000 7375 11000AG Peg S. Charbonnel 19/10/2018 3917 7593 11000 CH Cyg K. Graham 17/10/2018 3641 7370 545AG Peg J. Guarro 21/10/2018 3980 7763 9000 CH Cyg S. Charbonnel 17/10/2018 3917 7593 11000AG Peg D. Boyd 29/10/2018 3901 7380 1118 CH Cyg J. Guarro 21/10/2018 3980 7763 9000AG Peg J. Foster 31/10/2018 3700 7400 600 CH Cyg P. Somogyi 24/10/2018 3822 3979 5814AG Peg P. Somogyi 31/10/2018 8091 8788 2742 CH Cyg P. Somogyi 30/10/2018 3823 3980 5350AG Peg J. Guarro 04/11/2018 4053 7763 9000 CH Cyg J. Foster 31/10/2018 3700 7400 606AG Peg P. Berardi 09/11/2018 6374 6790 5618 CH Cyg J. Guarro 07/11/2018 4053 7763 9000AG Peg J. Foster 11/11/2018 3606 7401 529 CH Cyg P. Berardi 09/11/2018 6367 6786 5519AG Peg J. Foster 12/11/2018 6151 9600 736 CH Cyg J. Guarro 11/11/2018 3980 7763 9000AG Peg J. Foster 03/12/2018 6152 9676 806 CH Cyg P. Somogyi 11/11/2018 3822 3977 5192AG Peg J. Foster 04/12/2018 3701 7400 555 CH Cyg F. Teyssier 14/11/2018 4059 7395 11000AG Peg L. Franco 08/12/2018 3831 7231 543 CH Cyg J. Guarro 14/11/2018 3980 7763 9000AG Peg J. Guarro 14/12/2018 4053 7499 9000 CH Cyg F. Boubault 18/11/2018 4003 7502 1000AG Peg D. Boyd 24/12/2018 3902 7380 1108 CH Cyg F. Teyssier 18/11/2018 4060 7300 11000AXPer S. Charbonnel 05/10/2018 3917 7593 11000 CH Cyg J. Guarro 21/11/2018 4053 7763 9000AXPer S. Charbonnel 09/10/2018 4266 7593 11000 CH Cyg J. Guarro 24/11/2018 4053 7763 9000AXPer D. Boyd 09/10/2018 3901 7380 1010 CH Cyg J. Foster 26/11/2018 6102 9650 1043AXPer P. Somogyi 13/10/2018 4448 5164 1764 CH Cyg J. Foster 03/12/2018 6156 9672 825AXPer P. Somogyi 14/10/2018 5488 6200 2331 CH Cyg J. Guarro 03/12/2018 4053 7763 9000AXPer P. Berardi 19/10/2018 6362 6790 5634 CH Cyg J. Guarro 09/12/2018 4053 7499 9000AXPer D. Boyd 26/10/2018 3901 7380 1129 CH Cyg J. Guarro 14/12/2018 4053 7499 9000AXPer P. Somogyi 31/10/2018 8089 8787 2700 CH Cyg J. Guarro 19/12/2018 4053 7499 9000AXPer P. Berardi 09/11/2018 6378 6785 5961 CH Cyg J. Guarro 22/12/2018 4053 7499 9000AXPer J. Foster 10/11/2018 3700 7400 559 CI Cyg F. Teyssier 20/03/2018 4209 7395 11000AXPer F. Boubault 18/11/2018 4000 7501 1000 CI Cyg F. Teyssier 20/04/2018 4143 7395 11000AXPer D. Boyd 21/11/2018 3901 7379 1118 CI Cyg J. Guarro 21/08/2018 3980 7763 9000AXPer J. Foster 26/11/2018 6103 9651 1016 CI Cyg S. Charbonnel 18/10/2018 3917 7593 11000AXPer F. Sims 29/11/2018 3726 7275 937 CI Cyg J. Guarro 25/10/2018 3980 7763 9000AXPer J. Foster 01/12/2018 3641 7401 555 CI Cyg J. Foster 11/11/2018 3750 7401 550AXPer J. Foster 04/12/2018 3701 7400 564 CI Cyg J. Foster 12/11/2018 6102 9639 735AXPer L. Franco 08/12/2018 3855 7229 544 CI Cyg G. Martineau 14/11/2018 3925 7550 932AXPer F. Sims 13/12/2018 3726 7275 984 CI Cyg J. Foster 26/11/2018 6102 9650 1027AXPer D. Boyd 13/12/2018 3901 7379 1097 CI Cyg J. Foster 03/12/2018 6156 9670 837AXPer C. Buil 25/12/2018 5757 7261 1126 CI Cyg J. Guarro 03/12/2018 4053 7763 9000AXPer F. Campos 29/12/2018 3889 7428 1081 CI Cyg J. Guarro 10/12/2018 4053 7499 9000AXPer D. Boyd 29/12/2018 3901 7379 1107 CQ Dra V. Marik 18/11/2018 3681 7392 615AXPer F. Sims 30/12/2018 3727 7276 973 EF Aql D. Boyd 11/11/2018 3901 7380 1048BD Cam J. Foster 11/11/2018 6105 9570 844BD Cam J. Foster 12/11/2018 3726 7395 564BD Cam V. Marik 18/11/2018 3694 7392 609BF Cyg J. Guarro 02/10/2018 3980 7763 9000BF Cyg P. Somogyi 31/10/2018 8090 8789 2193BX Mon F. Campos 30/12/2018 3877 7425 970

Range Range

Id. Observer Date Res. Id. Observer Date Res.EG And G. Martineau 13/10/2018 3603 7404 1310 tcpj19544251+1722281K. Graham 20/08/2018 3705 7372 560EG And J. Foster 28/10/2018 3805 7395 576 tcpj19544251+1722281G. Martineau 04/10/2018 3603 7400 1116EG And J. Foster 26/11/2018 6102 9650 1019 tcpj19544251+1722281K. Graham 05/10/2018 3696 7384 555EG And F. Sims 19/12/2018 3726 7275 986 tcpj19544251+1722281P. Berardi 12/10/2018 4483 5503 1919EG And F. Teyssier 21/12/2018 4059 7395 11000 tcpj19544251+1722281U. Sollecchia 12/10/2018 6387 6766 8422EG And J. Guarro 22/12/2018 4053 7499 9000 tcpj19544251+1722281S. Charbonnel 18/10/2018 4036 7593 11000EG And F. Sims 31/12/2018 3726 7275 978 tcpj19544251+1722281P. Berardi 19/10/2018 6388 6744 5307EN Sgr F. Sims 11/10/2018 3970 7241 1047 tcpj19544251+1722281P. Somogyi 31/10/2018 8094 8792 2409EN Sgr F. Sims 15/10/2018 3950 7275 1038 UV Aur D. Boyd 17/11/2018 3901 7380 1117ER Del F. Campos 20/10/2018 3814 7348 940 UV Aur F. Sims 04/12/2018 3726 7275 980hen3-1768 T. Bohlsen 16/05/2018 3800 7399 1898 UV Aur D. Boyd 24/12/2018 3900 7380 1090hen3-1768 T. Bohlsen 27/05/2018 3800 7400 1534 V1261 Ori J. Foster 02/12/2018 6252 9650 764PU Vul F. Campos 20/10/2018 3813 7357 992 V1261 Ori F. Campos 29/12/2018 3881 7418 1051R Aqr F. Campos 03/10/2018 3835 7366 755 V1329 Cyg D. Boyd 22/10/2018 3902 7380 1120R Aqr F. Sims 05/10/2018 3706 7294 1032 V443 Her J. Foster 11/11/2018 3750 7401 554R Aqr F. Campos 21/10/2018 3819 7353 915 V443 Her J. Foster 12/11/2018 6207 9629 745R Aqr J. Guarro 24/10/2018 3980 7763 9000 V471 Per F. Campos 25/10/2018 3819 7356 936R Aqr F. Sims 25/10/2018 3726 7275 903 V471 Per F. Sims 07/11/2018 3726 7275 1002R Aqr J. Foster 28/10/2018 3805 7395 593 V471 Per J. Foster 10/11/2018 3606 7400 540R Aqr F. Sims 03/11/2018 3726 7275 957 V471 Per J. Foster 26/11/2018 6201 9601 1013R Aqr F. Sims 06/11/2018 3726 7275 1022 V471 Per J. Foster 01/12/2018 3766 7390 555R Aqr J. Guarro 07/11/2018 3980 7763 9000 V471 Per F. Sims 14/12/2018 3727 7276 984R Aqr P. Berardi 09/11/2018 6367 6789 5801 V471 Per F. Campos 29/12/2018 3889 7430 1031R Aqr J. Foster 11/11/2018 3750 7401 529 V471 Per F. Sims 31/12/2018 3727 7276 975R Aqr J. Foster 12/11/2018 6211 9550 724 V627 Cas F. Campos 20/10/2018 3815 7343 939R Aqr J. Foster 03/12/2018 6155 9671 823 V627 Cas D. Boyd 24/10/2018 3900 7380 1082R Aqr F. Sims 04/12/2018 3726 7275 976 V627 Cas F. Sims 13/12/2018 3726 7275 962R Aqr J. Foster 04/12/2018 3701 7400 554 V694 Mon P. Somogyi 06/10/2018 6503 6612 12258R Aqr F. Sims 13/12/2018 3725 7274 944 V694 Mon P. Somogyi 13/10/2018 6501 6610 15335R Aqr J. Guarro 20/12/2018 3980 7499 9000 V694 Mon P. Somogyi 14/10/2018 5489 6201 2283R Aqr F. Sims 29/12/2018 3726 7275 971 V694 Mon P. Somogyi 25/10/2018 6503 6613 13794R Aqr F. Campos 30/12/2018 3823 7364 943 V694 Mon P. Somogyi 31/10/2018 6503 6612 15498ss295 F. Sims 17/10/2018 3776 7276 992 V694 Mon P. Somogyi 01/11/2018 8096 8793 2819StHa 190 F. Campos 21/10/2018 3822 7358 1096 V694 Mon J. Foster 11/11/2018 6216 9572 840StHa 32 F. Sims 20/12/2018 3726 7270 986 V694 Mon J. Foster 12/11/2018 4050 7396 566StHa 32 F. Sims 30/12/2018 3726 7275 991 V694 Mon P. Somogyi 12/11/2018 6501 6611 15423StHa 55 J. Foster 10/11/2018 3801 7400 536 V694 Mon J. Foster 02/12/2018 6251 9651 793StHa 55 J. Foster 11/11/2018 6202 9571 836 V694 Mon J. Foster 04/12/2018 3701 7400 557SU Lyn J. Foster 10/11/2018 3801 7400 539 V694 Mon F. Campos 29/12/2018 3877 7425 998SU Lyn J. Foster 11/11/2018 6200 9568 814 Z And J. Foster 01/10/2018 6426 6699 9153SU Lyn J. Foster 25/11/2018 6101 9649 956 Z And T. Rodda 06/10/2018 3701 7401 613SU Lyn J. Foster 28/11/2018 3751 7400 560 Z And P. Berardi 12/10/2018 4483 5503 1878SU Lyn J.Coffin 10/12/2018 3801 7400 562 Z And P. Somogyi 12/10/2018 6500 6610 15287SU Lyn F. Sims 14/12/2018 3727 7276 962 Z And S. Charbonnel 17/10/2018 3917 7593 11000SU Lyn F. Sims 31/12/2018 3726 7275 948 Z And J. Guarro 24/10/2018 3980 7763 9000

Z And F. Sims 06/11/2018 3727 7275 1009Z And J. Guarro 06/11/2018 3980 7763 9000Z And D. Boyd 18/11/2018 3901 7380 1114Z And G. Martineau 22/11/2018 3603 7598 1296Z And F. Sims 29/11/2018 3727 7276 1023Z And J. Guarro 10/12/2018 4053 7499 9000Z And F. Sims 30/12/2018 3726 7275 982Z And F. Campos 30/12/2018 3836 7357 1111

Range Range


Symbiotics observed in October-December, 2018 2/2

AG Dra 2018

Coordinates (2000.0)R.A. 16 01 41.0Dec +66 48 10.1Mag V 9.8

SYMBIOTICS

Continuous observations of AG Dra upon the request of J. Merc and R. GàlisAfter the burst of AG Dra has returned to quiescent state. Ongoing survey until the next outburst expected during Spring 2019


9

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102458100 2458190 2458280 2458370 2458460 2458550

AG Dra (V)

2440000 2442000 2444000 2446000 2448000 2450000 2452000 2454000 2456000 2458000 2460000

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Ma

gn

itu

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1960 1970 1980 1990 2000 2010 20208

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AAVSO long term lightcurve - Visual (15 days mean)

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erg

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10-12 AG Dra 2018-12-12 20:55:54 R = 1107 D. Boyd

AG DraSYMBIOTICS


6400 6500 6600 6700 6800 6900 7000 7100 7200

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AG Dra 2018-11-24 17:51:28 R = 4498 Fran Campos

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AG Dra 2018-10-19 18 R = 11000 S. Charbonnel

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AG Dra 2018-10-12 18:14:39 R = 11000 Joan Guarro Flo


AG Dra in 2018 Equivalent widths from Echelle spectraSYMBIOTICS

8100 8200 8300 8400 8500

JD - 2450000

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120AG Dra - EW H alpha

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JD - 2450000

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JD - 2450000

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8100 8200 8300 8400 8500

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30

40

50AG Dra - EW He II 4686

8100 8200 8300 8400 8500

JD - 2450000

4

5

6

7

8

9

10

11

12AG Dra - EW Raman OVI 6830

AG PegSYMBIOTICS


7

7.5

8

8.5

9

9.52457000 2457365 2457730 2458095 2458460 2458825

AG Peg (V)

Coordinates (2000.0)R.A. 21 51 02.0Dec +12 37 32.1Mag V 8.9 (2019-01)

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

2

4

6

8

10

rela

tive

in

ten

sity

AG Peg 2018-12-08 17:08:46 R = 543 L. Franco


AG PegSYMBIOTICS

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

2

2.5

Flu

x [

erg

.cm

-2.s

-1.Å

-1]

10-11 AG Peg 2018-10-29 19:49:34 R = 1118 D. Boyd

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

2

flu

x (

erg

cm

- 2 s

- 1 A

- 1)

10-11 AG Peg 2018-12-24 18:34:17 R = 1108 D. Boyd

Flux calibrated spectra obtained by David Boyd (LISA R = 1000)

AG PegSYMBIOTICS


6400 6500 6600 6700 6800

Wavelength (A)

0

5

10

15

20

25

rela

tive

in

ten

sity

AG Peg 2018-11-09 17:35:08 R = 5618 Paolo Berardi

-1000 -500 0 500 1000

velocity (km/s)

0

5

10

15

20Halpha 2018-11-09

8100 8200 8300 8400 8500 8600 8700 8800

Wavelength (A)

0

0.5

1

1.5

2

rela

tive

in

ten

sity

AG Peg 2018-10-31 21:27:06 R = 2742 P. Somogyi

Near IR obtained by Peter Somogyi with Lhires III 600 l/mm OI in emission, Ca II in absorption

H alpha range obtained by Paolo Berardi with Lhires III 1200 l/mm

AG PegSYMBIOTICS


-1000 -500 0 500 1000

velocity (km/s)

0

5

10

15

20

25

30

arb

itra

ry u

nit

AG Peg H alpha

2018-10-01

2018-10-19

2018-10-21

2018-11-04

2018-12-14

-500 -250 0 250 500

velocity (km/s)

0

5

10

15

20

25

30

arb

itra

ry u

nit

AG Peg H beta

2018-10-01

2018-10-19

2018-10-21

2018-11-04

2018-12-14

-500 -250 0 250 500

velocity (km/s)

0

2

4

6

8

10

12

arb

itra

ry u

nit

AG Peg He I 5875

2018-10-01

2018-10-19

2018-10-21

2018-11-04

2018-12-14

-500 -250 0 250 500

velocity (km/s)

0

5

10

15

20

25

30

35

40

arb

itra

ry u

nit

AG Peg He II 4686

2018-10-01

2018-10-19

2018-10-21

2018-11-04

2018-12-14

-500 -250 0 250 500

velocity (km/s)

0

1

2

3

4

5

6

arb

itra

ry u

nit

AG Peg [Fe VII] 6087

2018-10-01

2018-10-19

2018-10-21

2018-11-04

2018-12-14

6800 6820 6840 6860

Wavelength (A))

0

1

2

3

4

5

6

rela

tive

in

ten

sity

Raman OVI 6830

2018-10-01

2018-10-19

2018-10-21

2018-11-04

2018-12-14

2018-10-01

2018-10-19

2018-10-21

2018-11-04

2018-12-14

Line profiles from Echelle spectra obtained by Joan Guarro and Stephane Charbonnel

AX PerSYMBIOTICS

Coordinates (2000.0)R.A. 01 36 22.7Dec +54 15 02.4Mag 11.5 (2019-01)

10.5

11

11.5

12

12.52457500 2457865 2458230 2458595

AX Per (V)

6000 6500 7000

Wavelength (A)

0

5

10

15

20

rela

tive

in

ten

sity

AX Per 2018-12-25 19:12:29 R = 1126 C Buil

H alpha range with the prototype UVEX3


V mag with respectect to phase. Current cycle: brown squares.Note the strong variations of the eclipse profiles.

AX PerSYMBIOTICS

Near IRJames Foster: LISA R = 1000 Peter Somogyi: Lhires III 600 l/mm R = 2700

7000 7500 8000 8500 9000 9500

Wavelength (A)

0

1

2

3

4

5

6

7

rela

tive

in

ten

sity

AX Per 2018-11-26 06:15:04 R = 1016 James R. Foster

O I in emission, Ca II triplet in absortion


8100 8200 8300 8400 8500 8600 8700 8800

Wavelength (A)

0

0.5

1

1.5

2

rela

tive

in

ten

sity

AX Per 2018-10-31 23:08:11 R = 2700 P. Somogyi

AX PerSYMBIOTICS

6400 6500 6600 6700

Wavelength (A)

0

10

20

30

40

50

rela

tive

in

ten

sity

AX Per 2018-11-09 19:40:35 R = 5961 Paolo Berardi

-1000 -500 0 500 1000

velocity (km/s)

0

5

10

15

20

25

30

35Halpha 2018-11-09

-1000 -500 0 500 1000

velocity (km/s)

0.5

1

1.5

2

2.5

3HeI6678 2018-11-09

Red range by paolo Berardi with Lhires III 1200 l/mm R = 6000


4500 4600 4700 4800 4900 5000 5100

Wavelength (A)

0

5

10

15

20

rela

tive

in

ten

sity

AX Per 2018-10-13 22:42:10 R = 1764 P. Somogyi


Hb region - Peter Somogyi - Lhires III 600 l/mm

AX PerSYMBIOTICS

-1000 -500 0 500 1000

velocity (km/s)

0

10

20

30

40

50

60Halpha 2018-10-05

-1000 -500 0 500 1000

velocity (km/s)

0

10

20

30

40

50

60

70

80Hbeta 2018-10-05

-1000 -500 0 500 1000

velocity (km/s)

0

5

10

15

20

25

30HeI5876 2018-10-05

-1000 -500 0 500 1000

velocity (km/s)

0

1

2

3

4

5

6HeI6678 2018-10-05

-1000 -500 0 500 1000

velocity (km/s)

0

10

20

30

40

50HeII4686 2018-10-05

-1000 -500 0 500 1000

velocity (km/s)

0

2

4

6

8

10[FeVII]6087 2018-10-05

-400 -200 0 200 400

velocity (km/s)

0

1

2

3

4

5

6

7[OIII]5007 2018-10-05


5000 5010 5020

Wavelength (A)

0

2

4

6

8

10re

lative

in

ten

sity

AX Per 2018-10-05 R = 11000 S. Charbonnel

Echelle spectrum - R = 11000Stéphane Charbonnel 2018-10-05 Phase = 0898 (Fekel & al., 2000)

Note the double peaked [OIII] 5007 with FWZI ~ 180 km.s-1 and ~ 75 km.s-1 netween the peaks. The center of the line is shift by 169 km-s-1 to the rest wavelength (-52 km.s-1 with respect to the systemic velocity).Such [OIII] profile is uncommon in clas-sical symbiotics.

AX PerSYMBIOTICS


4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

2

Flu

x [

erg

.cm

-2.s

-1.Å

-1]

10-12 AX Per 2018-12-29 20:27:02 R = 1107 D. Boyd

BD Cam

Coordinates (2000.0)R.A. 03 42 09.3Dec +63 13 00.0Mag

SYMBIOTI

CS


6500 7000

Wavelength (A)

0

0.5

1

1.5

2

2.5

3

rela

tive

in

ten

sity

BD Cam 2018-11-11 11:18:16 R = 844 James R. Foster

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

2

rela

tive

in

ten

sity

BD Cam 2018-11-18 22:29:34 R = 609 V. Marik

BF Cyg


SYMBIOTICS


99.510

10.511

11.512

12.513

13.5142451700 2455350 2459000

BF Cygni (V)

9

9.5

10

10.5

112458200 2458300 2458400

BF Cygni (V)

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

5

10

15

rela

tive

in

ten

sity

BF CYG 2018-10-02 19:37:24 R = 11000 J. Guarro

-1000 -500 0 500 1000

velocity (km/s)

0.5

1

1.5

2

2.5

3FeII4924 2018-10-02

-1000 -500 0 500 1000

velocity (km/s)

0

5

10

15

20Halpha 2018-10-02

-1000 -500 0 500 1000

velocity (km/s)

0

1

2

3

4

5

6

7Hbeta 2018-10-02



BF CygSYMBIOTICS

8100 8200 8300 8400 8500 8600 8700 8800

Wavelength (A)

0.6

0.8

1

1.2

1.4

1.6

rela

tive

in

ten

sity

BF Cyg 2018-10-31 17:53:50 R = 2193 P. Smogyi

Near IR Spectrum obtained by Peter Somogyi (Lhires IIII, 600 l/mm)OI l 8448 Å and Ca II ll 8498, 8542, 8749 Å in emission

SYMBIOTICS

BX Mon

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

2

2.5

rela

tive

in

ten

sity

BX Mon 2018-12-30 00:01:32 R = 970 F. Campos

Coordinates (2000.0)R.A. 19 23 53.5Dec +29 40 29.17Mag 9.6


CH Cyg

Coordinates (2000.0)R.A. 19 24 33.1Dec +50 14 29.1Mag ~ 7.2 (2017-07)

SYMBIOTICS

Ongoing campaign upon the request of Augustin SkopalAt least one spectrum a month (high resolution and low resolution, with a cor-rect atmospheric response)


4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

1

2

3

4

rela

tive

in

ten

sity

CH Cyg 2018-10-14 16:55:48 R = 524 T. Kantola

6

7

8

92457000 2457180 2457360 2457540 2457720 2457900 2458080 2458260 2458440 2458620

CH Cygni (V)

After its darkening event in June-July, CH Cygni recovered before declining monotically to mag V ~8,8 in 2019, January.


CH CygSYMBIOTICS

3820 3840 3860 3880 3900 3920 3940 3960 3980Wavelength (A))

0

2

4

6

8

10

12

14

16

18

20

rela

tive

in

ten

sity

CH Cyg P. Somogyi

2018-09-08

2018-09-15

2018-09-28

2018-09-29

2018-09-30

2018-10-05

2018-10-06

2018-10-12

2018-10-14

2018-10-24

2018-10-30

2018-11-11

6

7

8

92458200 2458260 2458320 2458380 2458440 2458500 2458560

CH Cygni (V)Near UV spectra during the decline from JD 2458370 (mag V ~6.75) to JD 2458434 (mag V ~ 7.7)

Peter Somogyi - Lhires III 600 l/mm - R = 2000

ARAS Eruptive Stars Information Letter #40 2018-04 - p. 27 ARAS Eruptive Stars Information Letter #40 2018-04 - p. 27

3820 3840 3860 3880 3900 3920 3940 3960 3980Wavelength (A))

0

2

4

6

8

10

12

14

16

18

20

rela

tive

in

ten

sity

CH Cyg P. Somogyi

2018-09-08

2018-09-15

2018-09-28

2018-09-29

2018-09-30

2018-10-05

2018-10-06

2018-10-12

2018-10-14

2018-10-24

2018-10-30

2018-11-11

CH Cyg Echelle spectraSYMBIOTICS


6

7

8

92458200 2458260 2458320 2458380 2458440 2458500 2458560

CH Cygni (V)

Date JD Observer10/08/2018 2458341.928 JGF11/08/2018 2458342.942 JGF13/08/2018 2458344.885 JGF14/08/2018 2458345.888 JGF15/08/2018 2458346.896 JGF18/08/2018 2458349.871 FMT 18/08/2018 2458349.948 JGF19/08/2018 2458350.936 JGF20/08/2018 2458351.228 LES20/08/2018 2458351.884 JGF21/08/2018 2458352.901 JGF24/08/2018 2458355.917 JGF25/08/2018 2458356.912 JGF26/08/2018 2458357.888 JGF27/08/2018 2458358.869 JGF13/09/2018 2458375.883 JGF14/09/2018 2458376.818 JGF17/09/2018 2458379.938 JGF18/09/2018 2458380.802 FMT 19/09/2018 2458381.855 JGF20/09/2018 2458382.858 JGF23/09/2018 2458385.821 JGF25/09/2018 2458387.814 JGF26/09/2018 2458388.863 JGF27/09/2018 2458389.822 JGF28/09/2018 2458390.808 JGF28/09/2018 2458390.884 FMT 29/09/2018 2458391.804 JGF29/09/2018 2458391.858 OGA30/09/2018 2458392.831 JGF30/09/2018 2458392.831 JGF01/10/2018 2458393.808 JGF12/10/2018 2458404.899 JGF16/10/2018 2458408.783 FMT 17/10/2018 2458409.928 SCH21/10/2018 2458413.769 JGF07/11/2018 2458430.839 JGF11/11/2018 2458434.828 JGF14/11/2018 2458437.804 FMT14/11/2018 2458437.843 JGF18/11/2018 2458441.800 FMT21/11/2018 2458444.841 JGF24/11/2018 2458447.764 JGF03/12/2018 2458456.770 JGF09/12/2018 2458462.754 JGF14/12/2018 2458467.747 JGF19/12/2018 2458472.766 JGF22/12/2018 2458475.735 JGF

Log of observations

JGF Joan Guarro FloFMT François TeyssierSCH Stéphane CharbonnelOGA Olovier Garde

-500 -250 0 250 500

velocity (km/s)

0

5

10

15

20

25

30

35

40

45

50

55

arb

itra

ry u

nit

CH Cyg H beta

2018-08-10

2018-08-11

2018-08-13

2018-08-14

2018-08-15

2018-08-18

2018-08-18

2018-08-19

2018-08-20

2018-08-20

2018-08-21

2018-08-24

2018-08-25

2018-08-26

2018-08-27

2018-09-13

2018-09-14

2018-09-17

2018-09-18

2018-09-19

2018-09-20

2018-09-23

2018-09-25

2018-09-26

2018-09-27

2018-09-28

2018-09-28

2018-09-29

2018-09-29

2018-09-30

2018-10-01

2018-10-12

2018-10-17

2018-10-21

2018-11-07

2018-11-11

2018-11-14

2018-11-14

2018-11-18

2018-11-21

2018-11-24

2018-12-03

2018-12-09

2018-12-14

2018-12-19

2018-12-22

-500 -250 0 250 500

velocity (km/s)

0

5

10

15

20

25

30

35

40

45

50

arb

itra

ry u

nit

CH Cyg O[I] 6300

2018-08-10

2018-08-11

2018-08-13

2018-08-14

2018-08-15

2018-08-18

2018-08-18

2018-08-19

2018-08-20

2018-08-20

2018-08-21

2018-08-24

2018-08-25

2018-08-26

2018-08-27

2018-09-13

2018-09-14

2018-09-17

2018-09-18

2018-09-19

2018-09-20

2018-09-23

2018-09-25

2018-09-26

2018-09-27

2018-09-28

2018-09-28

2018-09-29

2018-09-29

2018-09-30

2018-10-01

2018-10-12

2018-10-17

2018-10-21

2018-11-07

2018-11-11

2018-11-14

2018-11-14

2018-11-18

2018-11-21

2018-11-24

2018-12-03

2018-12-09

2018-12-14

2018-12-19

2018-12-22

-500 -250 0 250 500

velocity (km/s)

0

5

10

15

20

25

arb

itra

ry u

nit

CH Cyg [O III] 5007

2018-08-10

2018-08-11

2018-08-13

2018-08-14

2018-08-15

2018-08-18

2018-08-18

2018-08-19

2018-08-20

2018-08-20

2018-08-21

2018-08-24

2018-08-25

2018-08-26

2018-08-27

2018-09-13

2018-09-14

2018-09-17

2018-09-18

2018-09-19

2018-09-20

2018-09-23

2018-09-25

2018-09-26

2018-09-27

2018-09-28

2018-09-28

2018-09-29

2018-09-29

2018-09-30

2018-10-01

2018-10-12

2018-10-17

2018-10-21

2018-11-07

2018-11-11

2018-11-14

2018-11-14

2018-11-18

2018-11-21

2018-11-24

2018-12-03

2018-12-09

2018-12-14

2018-12-19

2018-12-22


Evolution of selected mlines during the decline



5880 5890 5900Wavelength (A))

0

5

10

15

20

25

rela

tive

in

ten

sity

CH Cyg

2018-08-10

2018-08-11

2018-08-13

2018-08-14

2018-08-15

2018-08-18

2018-08-18

2018-08-19

2018-08-20

2018-08-20

2018-08-21

2018-08-24

2018-08-25

2018-08-26

2018-08-27

2018-09-13

2018-09-14

2018-09-17

2018-09-18

2018-09-19

2018-09-20

2018-09-23

2018-09-25

2018-09-26

2018-09-27

2018-09-28

2018-09-28

2018-09-29

2018-09-29

2018-09-30

2018-10-01

2018-10-12

2018-10-17

2018-10-21

2018-11-07

2018-11-11

2018-11-14

2018-11-14

2018-11-18

2018-11-21

2018-11-24

2018-12-03

2018-12-09

2018-12-14

2018-12-19

2018-12-22

-500 -250 0 250 500

velocity (km/s)

0

5

10

15

20

25

arb

itra

ry u

nit

CH Cyg He I 5875

2018-08-10

2018-08-11

2018-08-13

2018-08-14

2018-08-15

2018-08-18

2018-08-18

2018-08-19

2018-08-20

2018-08-20

2018-08-21

2018-08-24

2018-08-25

2018-08-26

2018-08-27

2018-09-13

2018-09-14

2018-09-17

2018-09-18

2018-09-19

2018-09-20

2018-09-23

2018-09-25

2018-09-26

2018-09-27

2018-09-28

2018-09-28

2018-09-29

2018-09-29

2018-09-30

2018-10-01

2018-10-12

2018-10-17

2018-10-21

2018-11-07

2018-11-11

2018-11-14

2018-11-14

2018-11-18

2018-11-21

2018-11-24

2018-12-03

2018-12-09

2018-12-14

2018-12-19

2018-12-22

Emission of Na I D increases


CH Cyg Echelle spectra Equivalent widthsSYMBIOTICS

8300 8350 8400 8450 8500

JD - 2450000

0

10

20

30

40

50CH Cyg - EW H alpha

8300 8350 8400 8450 8500

JD - 2450000

0

10

20

30CH Cyg - EW H beta

8300 8350 8400 8450 8500

JD - 2450000

0

2

4CH Cyg - EW He I 5876

8300 8350 8400 8450 8500

JD - 2450000

0

1

2

3

4

5

6

7

8

9CH Cyg - EW [OIII] 5007

8300 8350 8400 8450 8500

JD - 2450000

0

1

2

3

4

5

6CH Cyg - EW [OI] 6300


CQ DraSYMBIOTICS

Coordinates (2000.0)R.A. 12 30 06.7Dec +69 12 04.Mag V 4.9


4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

2

rela

tive

in

ten

sity

CQ Dra 2018-11-18 22:52:51 R = 615 V. Marik

EF AqlSYMBIOTICS


Coordinates (2000.0)R.A. 19 51 51.7Dec -05 48 16.7Mag V 12.8


4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

2

2.5

3

3.5

Flu

x [

erg

.cm

-2.s

-1.Å

-1]

10-13 EF Aql 2018-11-11 17:53:26 R = 1048 D. Boyd

The long period variable EF Aql (12.4 < V < 15.5) was classified as a Mira symbiotic in 2014 by Margon & al. (2015) who discovered [OIII] in emission. The photometric period is 329.4 days (Richwine et al. (2005). EF Aql is one the few symbiotics stars showing flicker-ing (Zamanov, 2017).

Davis Boyd obtained a flux calibrated spectrum of this poorly stud-ied symbiotic star.

The discovery spectrum (Margon & al., 2015)

EG AndSYMBIOTICS


4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

rela

tive

in

ten

sity

EG And 2018-10-28 08:34:15 R = 576 James R. Foster

6500 7000 7500 8000 8500 9000 9500

Wavelength (A)

0

0.5

1

1.5

2

2.5

rela

tive

in

ten

sity

EG And 2018-11-26 07:13:47 R = 1019 James R. Foster


4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

rela

tive

in

ten

sity

EG And 2018-10-13 20:47:21 R = 1310 Martineau Buchet

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

rela

tive

in

ten

sity

EG And 2018-12-19 03:35:40 R = 986 Forrest Sims

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

2

rela

tive

in

ten

sity

EG And 2018-12-31 02:00:13 R = 978 Forrest Sims

EG AndSYMBIOTICS


EG AndSYMBIOTICS

-1000 -500 0 500 1000

velocity (km/s)

0.5

1

1.5

2

2.5

3Halpha 2018-12-21

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

2

2.5

3

rela

tive

in

ten

sity

EG And 2018-12-21 17:16:56 R = 11000 F Teyssier

-500 0 500

velocity (km/s)

0.5

1

1.5

2

2.5Hbeta 2018-12-21

-500 0 500

velocity (km/s)

0.6

0.7

0.8

0.9

1

1.1

1.2

1.3

1.4HeI5876 2018-12-21


ER DelSYMBIOTICS

Coordinates (2000.0)R.A.DecMag V 10.2 (2018-07)

4000 4500 5000 5500 6000 6500 7000

Wavelength (A)

0

0.5

1

1.5

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ER Del 2018-10-20 20:49:44 R = 940 F. Campos


Hen 3-1768 = ASAS J195948–8252.7SYMBIOTICS

Coordinates (2000.0)R.A. 19 59 48.4Dec -82 52 37.5Mag V 11.7 (2018-06)

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10-12 Hen 3-1768 2018-05-16 13:27:54 R = 1898 T. Bohlsen

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10-13 Hen 3-1768 2018-05-16 13:27:54 R = 1898 T. Bohlsen

http://www.astrosurf.com/aras/Aras_DataBase/Symbiotics/Hen3-1768.htm

A new bright symbiotic star from Adrian Lucy's list (see p. ) identified with spectra obtained by Terry Bohlsen.He II line and Raman OVI clearly identify the target as a symbiotic (Belczinski & al., 2000). The giant star is K type, making Hen 3-1768 as a member of the yellow symbiotic starsSee the reserch note: http://iopscience.iop.org/article/10.3847/2515-5172/aaf71c/meta


SYMBIOTICS



HbHa1704-058 = Vend 47 New symbiotic star

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tcpj19544251+1722281 2018-10-04 20:46:17 R = 1116 Martineau Buchet

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TCP J19544251+1722281 2018-10-05 00:29:28 R = 555 K Graham

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132458330 2458360 2458390 2458420 2458450 2458480 2458510The new symbiotic star (see Information letter #39)

is declining. Raman OVI increase while [Fe VII] and [O III] are still very weak, if present.

SYMBIOTICS


HbHa 1704-058

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TCP J19544251+1722281 2018-10-31 19:45:30 R = 2409 P. Somogyi

Near IR with Lhires III 600 l/mm R = 2500 by Peter Somogyi. OI l 8447, Ca II ll 8498, 8542, 8662 in emission

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80Halpha 2018-10-12

Ha profileUmbert Sollecchia R = 8000

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80Halpha 2018-10-19

SYMBIOTICS


HbHa 1704-058

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TCP J19544251+1722281 2018-10-12 17:26:47 R = 1919 Paolo Berardi

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HbHa 1704-058 SYMBIOTICS


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TCP J19544251+1722281 2018-10-18 19:07:46 R = 11000 S. Charbonnel

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2018-10-18 19:0 R = 11000

[OIII] very faint if present

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1.8[FeVII]6087 2018-10-18

[Fe VII] still very faintThe narrow line is Fe II l 6084

The equivalent width of Raman OVI 6830 is about - 3.3

PU VulSYMBIOTICS



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PU Vul 2018-10-20 18:37:12 R = 992 F. Campos

R AqrSYMBIOTICS



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R Aqr


R AqrSYMBIOTICS

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R Aqr

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R Aqr F. Sims

2018-10-05

2018-10-25

2018-11-03

2018-12-04

2018-12-13

2018-12-29

Series obtained by Woodu Sims during the decline with LISA (R =1000) showing the classical strengthening of the various lines according to the continuum

SYMBIOTICS


R Aqr

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R Aqr 2018-11-09 18:46:37 R = 5801 Paolo Berardi

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25Halpha 2018-11-09

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3.5[NII]6583 2018-11-09 Ha range by Paolo Berardi

with LHIRES III 1200l/mm

StHa 32SYMBIOTICS

Coordinates (2000.0)R.A. 04 37 45.6Dec -01 19 11.89Mag V 12.7


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StHa 32 2018-12-20 03:41:00 R = 986 Forrest Sims

StHa 55SYMBIOTICS

Coordinates (2000.0)R.A. 05 46 42.07Dec +06 43 47.07Mag V

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StHa 55 2018-11-10 11:47:06 R = 536 James R. Foster

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StHa 55 2018-11-11 11:38:55 R = 836 James R. Foster


The carbon star StHa 55 observed by James Foster in visible (ALPY R = 600) and in near IR (LISA R = 1000). Ha in emission. Note the significant difference of resolution between the two spectroscopes.

StHa 190SYMBIOTICS



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StHa 190 2018-10-21 18:22:16 R = 1096 F. Campos

SU LynSYMBIOTICS

Coordinates (2000.0)R.A. 06 42 55.1Dec +55 28 27.2Mag V ~ 8.5


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SU Lyn 2018-12-10 00:48:45 R = 562 J. Coffin

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SU Lyn 2018-12-14 06:23:35 R = 962 Forrest Sims

UV AurSYMBIOTICS

Coordinates (2000.0)R.A. 05 21 48.9Dec +32 30 40.1Mag 9 (2019-01)


AAVSO Vis band lightcurve (15 days mean) and ARAS spec-tra (blue dots)


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112457700 2458065 2458430 2458795

UV Aur (V)

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10-11 UV Aur 2018-11-17 22:14:04 R = 1117 D. Boyd

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10-12 UV Aur 2018-12-24 19:57:49 R = 1090 D. Boyd

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2018-11-17.9262018-12-24.832

UVAur D.Boyd

UV AurSYMBIOTICS

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UV Aur 2018-12-04 03:59:23 R = 980 Forrest Sims


V443 HerSYMBIOTICS



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V0443 Her 2018-11-11 02:52:25 R = 554 James R. Foster

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V0443 Her 2018-11-12 02:39:09 R = 745 James R. Foster

V471 PerSYMBIOTICS



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V0471 Per 2018-10-11 11:32:05 R = 651 James R. Foster

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V471 Per 2018-12-29 19:43:50 R = 700 F. Campos

V471 PerSYMBIOTICS

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V471 Per 2018-11-07 03:10:18 R = 1002 Forrest Sims


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V471 Per 2018-12-31.115 5421 s (9 x 600 s) Forrest Sims

Hga

mm

a 43

40.4

6[O

III]

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.21

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II 46

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8

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ta 4

861.

363

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I] 49

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.84

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I 587

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I 667

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[Ar I

II] 7

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V471 Per 2018-12-31.115 5421 s (9 x 600 s) Forrest Sims

He

I 447

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8

[N II

] 575

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I 587

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] 654

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[N II

] 658

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I 667

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I 706

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[Ar I

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V471 Per 2018-12-31.115 Forrest SimsAGDra 2018-12-12.872 D.Boyd


Comparison with the yellow symbiotic AG Dra

V471 PerSYMBIOTICS

V627 CasSYMBIOTICS



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10-13 V627 Cas 2018-10-24 17:41:38 R = 1082 D. Boyd

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V627 Cas 2018-12-13 03:06:21 R = 964 Forrest Sims

V694 Mon = MWC 560SYMBIOTICS

Coordinates (2000.0)R.A. 07 25 51.28Dec -07 44 08.07Mag 9.2


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112457100 2457465 2457830 2458195 2458560 2458925

V694 Mon

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V694 Mon 2018-12-29 22:46:18 R = 998 F. Campos

V694 Mon in high luminosityThe shape of Balmer lines is un-common with the disappearance of the usual broad absorptions.Fe II, HeI and Balmer lines shows P Cyg profiles with maximum ab-sorptions at ~ -100 km.s-1


Spectroscopic Observations of V694 Mon (= MWC 560) during its recent outburstATel #12231;Alessandra Azzollini, Marco Bellomo, Giovanni Leidi, Tommaso Migliorini, Marco Monaci (Dept. of Physics, Univ. of Pisa), Peter Somogyi (Tata, Hungary and ARAS Group)on 20 Nov 2018; 01:42 UTCredential Certification: S. N. Shore ([email protected])Spectra were obtained on 2018 Nov. 19.1 UT at Pisa using a 280 cm C11 telescope with the LHIRES III at resolutions of about 1300 (total exposure time of 3600 sec; 4700-7700A) and 18000 (6430-6631A; total exposures times of 3600 sec at each resolution) and on 2018 Oct. 31.1 UT at Tata with a 30cm LH2400 telescope resolution of about 16000 (6502-6611A; exposure time of 5400 sec), thus bracketing the observation reported in ATel #12227. The S/N ratio was > 10 in the continuum with the Halpha peak at about 40+/-2 times the continuum. The Halpha profile shows broad, extended wings at 10 to 15 percent of the peak intensity extending to +/-1000 km/s. The Oct 31 Halpha profile shows a superimposed absorption with a blue edge at -300 km/s that had weakened by Nov. 19 but with the blue side of the emission decidedly asymmetric compared to the red wing (reversal of the profile shows the absorption extends to nearly zero vrad). The low resolution spectrum shows little evidence other than profile asymmetry for absorption at Halpha and Hbeta, aside from a complex of Fe II emission lines there is a pronounced presence of the neutral He lines. He I 4922 and 5013 are much stronger than Fe II 4923 and 5018; Fe II 5169 is present but weak. He I 5013, 5876, and 6678 show P Cyg profiles, even at low resolution, with a similar blue absorption velocity to that of Halpha but with a higher absorption to emission ratio (of order unity, for 5876 and 6678 allowing for the resolution of about 5A, the absorption component is weaker on 5013). Na I is in absorption, providing a check on the reality of the absorption feature at low resolution. Si II 6347, 6371 may be present but the low resolution spectrum is not sufficiently high quality to be sure. [O I] 6300 is not detected nor are there other obvious forbidden lines, Observations will be continuing as weather permits. The spectra are available at the ARAS Database.

A.R.A.S Spectral Data Base - Eruptive stars section

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V694 Mon 2018-10-14 03:00:31 R = 2283 P. Somogyi


He I l 5876 with a broad emission component (see ATel #12231)


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V694 Mon 2018-09-09 03:20:04 R = 1952 P. Somogyi

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10Hbeta 2018-09-09

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V694 Mon 2018-09-30 03:50: R = 1953 P. Somogyi

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10Hbeta 2018-09-30


Hb range obtained by Peter Somogyi with Lhires III (600 l/mm R ~2000)Fe II (42) lines shows a P Cygni profile (maximum absorption ~ -100 -120 km.s-1). He I 4922 5016 appears in absorption (see next page)

Hb profiles in the red part of the line, the flat component extends to + 1100 km.s-1


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Fe II 4924 Fe II 5018 Fe II 5169 |2019-01-12

Fe II 4924

Fe II 5018

Fe II 5169

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Fe II 4924 Fe II 5018 Fe II 5169 |2018-09-30

Fe II 4924

Fe II 5018

Fe II 5169


2018-09-30 : Peter Somogyi, Lhires III R = 2000, 2019-01-12 : Joan Guarro, Echelle R = 9000Fe II (42) multiplet with P Cygni profile - Maximum absorption ~ 100 km.s-1

The comparison of the Fe II lines l4924 and l5018 to l5169 shows the absorptions produced by He I l4922 and l5016.

05

1015202530354045

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6500 6510 6520 6530 6540 6550 6560 6570 6580 6590 6600 6610Wavelength (Angstrom)

2018-10-06.1432018-10-13.1272018-10-25.1052018-10-31.0872018-12-31.909

V694 Mon P. Somogyi

Ha regionR = 15000In October,Ha remains almost stable, with P Cygni profile (maximum absorption at -185 km.s-1) and broad pediestrial extended to 980 km.s-1 in the red. Late december, the absorption shifted to -105 km.s-1 and the broad component declined be-tween 700 and 980 km-1

Fe II l also table (RV = +15 km.s-1 ) in October is shifted by 20 km.s-1 (RV = 35 km.s-1) late Decem-ber

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2018-10-06.1432018-10-13.1272018-10-25.1052018-10-31.0872018-12-31.909

Fe II 6516.08 - V694 Mon P. Somogyi

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2018-10-06.1432018-10-13.1272018-10-25.1052018-10-31.0872018-12-31.909

v694 Mon PSO

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2018-10-06.1432018-10-13.1272018-10-25.1052018-10-31.0872018-12-31.909

H I 6562.801 - V694 Mon P. Somogyi

V694 Mon = MWC 560


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V694 Mon 2018-11-01 01:17:51 R = 2819 P. Somogyi

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V0694 Mon 2018-11-11 12:41:41 R = 840 James R. Foster


Near IR spectra by Peter Somogyi, with Lhires III 600 l/mm and James Foster with LISA (R = 1000) showing OI, Ca II triplets and Pascher lines in emission

V1261 OriSYMBIOTICS


Coordinates (2000.0)R.A. 05 22 18.6Dec -08 39 58.0Mag 6.8

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V1261 Ori 2018-12-02 09:58:31 R = 764 James R. Foster

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V1261 Ori 2018-12-29 21:41:07 R = 1051 F. Campos

V919 SgrSYMBIOTICS

Coordinates (2000.0)R.A. 19 03 45.1Dec -16 59 55.37Mag 13.1 (2018-10)


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V0919 Sgr 2018-10-12 03:55:28 R = 665 James R. Foster


V1329 CygSYMBIOTICS



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10-13 V1329 Cyg 2018-10-22 19:34:15 R = 1120 D. Boyd

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10-13 V1329 Cyg 2018-10-22 19:34:15 R = 1120 D. Boyd

Z AndSYMBIOTICS

Coordinates (2000.0)R.A. 23 33 39.5Dec 48 49 5.4Mag V 9.8 (2019-01)


Still declining after the outburst of January 2018.The magnitude is slightly above the pre-outburst value.

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Z And (V)

AAVSO V band (1 day mean) and ARAS psctra in blue

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Z And 2018-10-06 22:29:37 R = 613 Tony Rodda

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Z And 2018-10-11 09:02:21 R = 636 James R. Foster

Z And 2018SYMBIOTICS


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Z And 2018-10-12 20:31:15 R = 1878 Paolo Berardi

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Halpha 6562.801 - Z And 2018-10-12.942 PSO

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Z And 2018-10-17 23:19:26 R = 11000 S. Charbonnel



# Date Time JD OBS1 01/12/2017 22:17 2458089.46 JGF2 05/12/2017 20:48 2458093.4 JGF3 12/12/2017 18:19 2458100.32 JGF4 23/01/2018 18:48 2458142.34 JGF5 30/01/2018 19:28 2458149.35 JGF6 17/02/2018 18:45 2458167.3 FMT 7 21/02/2018 18:22 2458171.3 FMT 8 22/02/2018 18:34 2458172.3 FMT 9 25/02/2018 18:27 2458175.3 FMT

10 25/02/2018 23:42 2458175.52 LES11 27/02/2018 18:23 2458177.29 FMT 12 05/03/2018 18:33 2458183.28 JGF13 07/03/2018 18:32 2458185.29 FMT 14 08/03/2018 18:52 2458186.31 JGF15 30/06/2018 1:44 2458299.59 FMT 16 02/08/2018 23:37 2458333.51 FMT 17 04/08/2018 22:45 2458335.48 JGF18 23/08/2018 5:33 2458353.78 LES19 26/08/2018 21:55 2458357.44 JGF20 14/09/2018 21:14 2458376.43 JGF21 17/09/2018 19:58 2458379.35 FMT 22 20/09/2018 19:19 2458382.37 JGF23 26/09/2018 20:29 2458388.39 JGF24 28/09/2018 19:27 2458390.38 JGF25 17/10/2018 23:19 2458409.51 SCH26 24/10/2018 18:20 2458416.3 JGF27 06/11/2018 22:20 2458429.47 JGF28 10/12/2018 20:59 2458463.43 JGF29 07/01/2019 19:06 2458491.33 JGF30 11/01/2019 18:10 2458495.29 JGF

Jounal of Echelle observationsJGF: Joan Guarro FloFMT: François TeyssierLES: Tim LesterSCH: Stephane Charbonnel



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Z And 2018SYMBI

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Campaign: Suspected Symbiotics StarsSYMBIOTICS

This campaign is initiated by Adrian Lucy and Jeniffer Sokolovski (Columbia University). The aim is to de-tect symbiotic stars among a list of suspected tragets proposed by Adran Lucy.AAVSO Alert Notice https://www.aavso.org/aavso-alert-notice-650

One of the target has been clearly identified as a symbiotic star (see p. and the research paper bpublished by Lucy & al., based on spectra obtained by Terry Bohlsen)

Share results and check the status of the campaign on ARAS forum:http://spectro-aras.com/forum/viewtopic.php?f=37&t=2124


Observations

Name RA (2000.0) Dec (2000.0) V mag* M giant Em. Lines 05 09 10 11 12 01 02

1 GAIA DR2 4636654969717900032 01 50 49.53 -76 49 42.6 12.9 no 1

2 UCAC3 157:43452 06 55 51.36 -11 44 05.3 12.3 no 1

3 GDS J0731468-195434 07 31 46.82 -19 54 34.5 13.2

4 ASASSN-V_J081823.00-111138.9 08 18 23.00 -11 11 38.9 12.5 no 1

5 UCAC3 80:46364 08 34 45.15 -50 26 58.2 13.7 no 1

6 11 03 10.83 -83 57 11.3 11.2

7 12 01 20.93 79 20 14.7 12.3

8 GAIA DR2 4131587500273361280 16 39 59.65 -18 44 38.1 13.9

9 ASASSN-V J164007.54-382216.1 16 40 07.54 -38 22 16.1 13.86-14.74

10 GAIA DR2 6019720819446985984 16 45 31.78 -36 22 31.6 12.9

11 V2096 Oph 16 56 05.46 -24 06 37.0 12.9-14.0

12 ER Oph 17 00 42.14 -26 10 12.4 11.8-<14.8

13 ASASSN-V J170231.98-275954.2 17 02 31.98 -27 59 54.4 13.98-14.94

14 GAIA DR2 4334886650491663104 17 06 08.44 -10 58 33.0 14.3

15 SS 295 17 07 38.16 -07 44 48.6 13.1 1

16 V2525 Oph 17 15 05.27 -09 23 50.1 11.9-<15.1

17 GAIA DR2 4115021291723497088 17 17 45.67 -21 31 16.9 13.7

18 GSC 09276-00130 17 18 09 -67 57 26.0 13.6

19 GAIA DR2 4168021909706732672 17 25 26.34 -07 48 27.5 14.3

20 GAIA DR2 4111779763989583232 17 26 18.27 -22 12 46.4 14.1

21 GAIA DR2 4120809606303456896 17 27 08.69 -21 39 04.5 13.1

22 GAIA DR2 5919388180059095296 17 30 58.39 -56 29 53.4 12.6 no 1

23 ASASSN-V J173832.43-492840.2 17 38 32.42 -49 28 40.1 13.96-14.55

24 FASTT 1100 17 53 45.30 -01 07 46.8 14.04-14.30 1

25 GAIA DR2 4150446010182968192 17 56 04.34 -13 10 03.4 13.1 M4 1

26 GAIA DR2 4150099732733146112 17 59 43.87 -13 58 32.0 13.9

27 SY Cra 18 03 21.54 -42 37 56.8 13.0-16.5p

28 GAIA DR2 6345873798283774848 18 14 18.07 -85 59 06.5 11.7 no 1

29 GAIA DR2 4048168377818693632 18 28 31.28 -28 45 02.9 11.9 no 1

30 ASASSN-V J185421.70-274827.4 18 54 21.70 -27 48 27.8 12.89-13.63

31 EN Sgr 19 22 42.08 -13 59 56.5 11.95-14.61 H I 2 2

32 ASASSN-V J192916.53-224040.3 19 29 16.53 -22 40 40.3 12.52-13.02 M 3.5 Ha Hb 1

33 ASAS J195948-8252.7 19 49 48.4 -82 52 37.5 11.6 yes 2

2018 2019



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ASASSN -V J081823 2019-01-12 22:41:07 R = 872 FPC



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EN Sgr 2018-10-15 02:04:35 R = 1038 Forrest Sims

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T CrB in ARAS DataBase

Ha equivalent width - Long term variation from various sources.The current active stage (4) is stronger than previous ones (1 & 2). Data are missing to establish high state #3.

He II l 4686 equivalent width ARAS - Echelle spectra (R = 9000 to 13000)

He II l 4686 equivalent width ARAS - LISA spectra (R = 1000)

He II l 4686 equivalent width ARAS - Echelle + LISA spectra


1 2 3? 4

The symbiotic recurrent nova T CrB is still in high state characterized by strong emission lines and blue con-tinuum (Iijima, 1990).

T CrB in ARAS DataBaseSYMBIOTICS

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Flux calibtated spectra obtained by David Boyd with LISA ( R = 1000 )

The music of the spheres Steve Shore


Okay, I know it's not exactly an original title but the context -- I promise -- won't be usual. Please bear with me, you all know that one of the aims of these columns is to discuss the links between physical processes and what you see as spectros-copists.To start, consider what happens when you clap your hands (my apologies to all of you who are not North Americans, the ``Pelosi Clap'' has become iconic in the last weeks). Two constrain-ing converging surfaces force air to compress and when opened, that expands as a pressure wave. This simple wave, because the compression was slower than the sound speed, propagates at the speed of sound without changing shape. In other words, it isn't a shock wave (more on that later). Your ear or even your skin, as a deformable surface with imbedded nerves, detects this pres-sure variation and the CPU then cross correlates the directional properties of the detectors (your ear folds and parallax) and you ``hear''. Nothing pre-selects the frequency, there are no lines in the spectrum of the emitted sound, and depending on how the clap deforms your hands the whole spec-trum can shift. Its duration is essentially a pulse.

To dissect this further, you'll notice that this was a point-like source (the clap) that radiates into a non-selfgravitating medium. Each phase of the wave is a variation in the local pressure so the wave is acting like a nonstationary piston that pushes on the air and expands into the surround-ing volume with constant energy. Viscosity in the gas then dissipates some of the spectrum as heat (the highest frequencies) while the lower ones (for which the acceleration is lower) continue to be audible at greater distance. This simple ex-ample introduces, then, all of. the processes you need to pass to the next level of complexity, that of medium that selects certain frequencies -- an acoustic filter or resonator.

Now take a tube, one from paper towels will do, and hit one end while he other is open. Batting the air column, which is otherwise confined, is an answer to the Zen conundrum about the ``sound of one hand clapping''. The column is compressed and a wafer of air is sent down the tube. The

open end is instantaneously in pressure equi-librium with the surroundings before the wafer arrives. Bt once the compression hits, it's over-pressured inside the tube. This does work on the outer gas exactly as before but with a twist. This is an expanding wafer from what was originally a cylinder of gas so there's an overshoot and some of the impulse is reflected back into the tube. If the driving isn't merely impulsive, if there's some frequency of driving like a periodic piston on one end of the tube, the reverse-propagating com-pression (rarefaction) may resonantly encoun-ter the advancing wafer. Where they are out of phase, they partly cancel. I say partly because there's a difference in the amplitudes. The pro-cess continues for as long as there's driving. The open boundary of the tube guarantees that there isn't a node at the end, there's a net outward acceleration so the air continues to leave. But if, instead, you close both ends of the tube, or hold it near a wall, then the acceleration in return must reverse sign at the boundary and the wave that reverses will be in a different phase relation to the driving. You had this in early introductions to music and physics, think back to your infancy: the closed tube acts as if it has twice the wavelength of the open tube. The resonance condition is that there be exact phase matching at every point in the tube so harmonics will also resonate in a linear sequence as you change the driving fre-quency.

From French horns to making pasta

Now think of what happens if instead of a cylin-der, you use a cone. Now the relation between the frequency and the resonance condition becomes a bit more complicated. You see, the opening angle of a cone is constant so the surface of the outgoing wafer increases as a section of the surface of a sphere. The pressure necessar-ily drops because of this divergence, in contrast to the straight ``bore'' of the cylinder. So as you change the frequency, the relation between the resonances won't be linear. The boundary behav-ior remains the same. For open cones, the length of the lube appears shorter than for one that's closed.



As one last modification in your instrument, wake a cone whose opening is a function of distance from the source, for instance one that's self-similar such that the longer the tube is the larger the opening angle. You've not only made something very much like the plumbing of a French horn or Posthorn, you've come very close to what happens in a star.

In a musical instrument, the driving isn't a simple clap at the end of the tube. You blow a jet into the air column, injecting a turbulent flow because of the ripples generated at the jet (we've dis-cussed this a while back also for vortex generation in disks and turbulence). In effect, you are excit-ing the column with a broad spectrum of which some frequencies are resonant and therefore simultaneously amplify. Others are not heard unless you change the blowing pressure and the spectrum shifts and the higher pressure puts more power into. the higher frequencies. Forget the details (which are lovely and below you'll find some really good references), this selection for resonance depends on the tube length. Ro now put a different, more astronomical take on the matter, on Mars -- where the atmospheric com-position is different from Earth -- the sound speed is also different. So the relation between the wavelength and driving frequency -- the product of which is the acoustic phase velocity -- changes the effective length of the tube even if its geo-metric length is the same as on Earth. The physics is invariant, it's just that you won'r hear Brel or Callas or Beyonce sounding the same. Imagine, then, two tubes. One is the variable opening angle horn, the other a straight cylinder in which we somehow change the sound speed along the tube. The results can be fine tuned to be the same.

The assumption here has been that there's a single wave front and one source of excitation, the ``ac-tive'' end of the tube. One more pass is needed to reach the stars. Put a pot of water on the stove in preparation for cooking pasta. Even as you ready the other ingredients, so without watching the wa-ter every moment, you know when to dump the pasta into the water: you hear it. Or more pre-cisely put, you hear the sound produced from the

incompressible surface of the water locally driv-ing the surrounding air in the same way as a large ensemble of individual sources all of which are at different phases. Of course, there are overshoots (the surface has breaking bubbles) and things get really messy but the broad spectrum of oscillations drives a broad spectrum of responses -- you get a continuum of sound. You know, however, that the pot isn't infinitely large and the waves can form a resonant spectrum of surface deformations even amid this chaos, so there will be some frequencies present in the sound that have selectively higher power than others. The sound speed in the room is constant. The sound speed in the pot is con-stant. So the spectrum should be pretty much the same whenever you're boiling the water. Once it turns chaotic, the turbulence is pretty much invari-ant in time.

... and then to the stars

Imagine that the boiling water is, instead, the con-vective region in the envelope of a star. Take the outermost zone, where atomic hydrogen ionizes. Th hotter the photosphere the closer this is to the surface. Although the photosphere may not be convecting (think for now of an A-type star, not the Sun), the pressure waves generated by expansion and contraction of individual elements of the enve-lope gas will produce outward (and inward) propa-gating sound waves. Since the pressure and den-sity structure of the outer layers of a star depend on how much flux has to be transferred, there are inevitably variations of the temperature and den-sity such that they both decrease outward. This means the sound speed also changes. Ah, there's the key: the outer layers, when expanded, cool and fall back under gravity. So the restoring force is different than in the kitchen or instrument. The waves are responding to the pressure fluctuations with a characteristic free fall time and a variable internal sound speed. The spectrum of resonanc-es is very different, then, from the musical instru-ment but the physics is the same. These modes have a very complex distribution of characteristic response frequencies and, depending on the run of the pressure and temperature through the star, produce photospheric fluctuations with a different



spectrum that links to the gravity (mass and radius of the star) and its effective temperature.

There you have it: a star is a badly tuned musical instrument that has the form of a spherical pot of hydrogen in overall mechanical and thermal bal-ance while internally generating its own noise.

Now if the gravitational timescale, the freefall time, for the piston-driven layers happens to reach a res-onance with the the driving timecale, something very special happens: the whole layer can start to move synchronously. This is pulsation. It requires that the driver have the right amount of overlying mass to drive, the right driving frequency and the right response time for the overlying layers. But those conditions are met under remarkably broad conditions. You know these. Pulsating variable stars are found across the range of stellar types. Near the main sequence, they have relatively short periods (the d Sct and related variables, periods of about an hour) to the cooler, lower gravity (not lower mass, larger radius and higher luminosity) d Cep variables (with periods of days to weeks), to the Miras (with periods more like years). The more extended the star, the longer the characteristic gravitational response time because of the lower surface gravity, so the driver excites different reso-nances. More complicated variations than a single period are observed and because all of this is not precisely tuned, the form of the pulsation is not a single, regular mono-frequency wave. You just have to look at the light curve of an RR Lyr type ab to get a feel for this, or a Cepheid. The instabil-ity that coordinates the convective zone to be the driver depends on how the rate of energy trans-fer varies over this cycle and whether a convec-tive zone is itself resonant. Those details are more than we'll need for the rest of this discussion but they form the basis of the remarkable probe -- as-teroseismology -- that now opens a dynamical win-dow into stellar interiors by simple observations of the frequency spectrum of the light curves. This was a byproduct of Kepler and, now, TESS, and the original scope of COROT and MOST.

What all this has to do with what you might see as an astronomer

All pulsation is, therefore, the dynamical response of the different layers within the star -- and at the surface -- to internal changes in pressure. What-ever provokes that variation is not directly ob-served. Its effect on the medium is. For a large scale pulsation, like a Cepheid, the photosphere is lifted and falls back in a periodic fashion, driven by a synchronized piston. The same for all classes of regular, periodic pulsators. So when the surface is moving outward, you see a blue shift of the pho-tospheric lines. A part of the cycle later, the re-verse happens. The lines are formed over the hole visible surface so it's somewhat like an expanding or contracting sphere, the lines shift and broaden in the phases of maximum velocity. In binary sys-tems, where the tidal action of a companion can distort the pulsator sufficiently, a non-radial mode may occur. The same for a rapidly rotating star. Anything that ``breaks the symmetry'' changes the frequency spectrum and introduces different coor-dinated modes in the stellar envelope. Remember, a rapidly rotating star is oblate (polar squashing) so it has a different response at the poles and the equator. The complexity of the pulsation pattern also increases with rotation because any outward motion is affected by the Coriolis acceleration so the surface also resonates with a multiple of the rotation frequency. Not wanting to b confusing here, let me refer you to a weather image of the Earth. Where you have pressure fluctuations, you have vorticity. As we discussed for accretion disks, this yields additional frequencies in the response of a disk (or a star).

The final thing you see, and this is most dramatic in Mira variables, is that the amplitude of the pul-sational displacement may be enormous, a large fraction of the mean size of the star. This can launch shells of gas outward and produce steep-ening of the outwardly moving pressure waves to the point of becoming shocks. The dramatic ap-pearance of He I emission in RR Lyr stars at some phases of their pulsation, that some of you have observed, and the time variations of emission in RV Tau and Mira variables, bear witness to this strongly dissipative process. It's the same as you get with waves breaking on a beach, something



that you fortunately don't suffer in a concert hall. When the density changes so rapidly that there's a significant change during a single cycle of the pres-sure wave, it must steepen. The same for the am-plitude -- when the energy of the acoustic wave is very large relative to the thermal energy, or when the variation in the density is about the same as the mean of the background, the wave steepens and literally over-runs itself. This is a shock. The upstream medium is compressed when engulfed, radiates and then expands and cools.

In symbiotics, this process of large amplitude, pul-sationally-driven mass loss must govern the mass transfer rate onto the degenerate. When shells are launched, they don't have enormously high veloci-ties and may even fall back to the giant. But they also modulate the wind flow toward the compan-ion. Flow through the L1 (inner Lagrangian point, or the Roche surface) has to change if the underly-ing star is pulsating but how is a vast computation-al problem. Such stars, being far more deformed than by simple rotation, can't pulsate like spheres. They must have non-radial modes but what those are is anone's guess. Alas, you won't be able to see these, the companions in cataclysmics are either too faint or simply overwhelmed by the disk. Some evidence for this sort of pulsational modulation is known from the Wolf-Rayet stars, and O stars, where isolated narrow so-called discrete absorp-tion components have been observed to accelerate outward toward the terminal wind speed. In Be stars, some of the profile changes are likely driven by these pulsational effects at the photosphere, a drumhead that shears relative to the surrounding air and could be important in launching "decre-tion disks''. The mechanism, while not understood well, is hypothesized to provide more angular mo-mentum to the near-surface laters than they would have if circulating normally (Keplerian orbits). Hence, with the excess angular momentum, they start drifting outward and viscosity does the rest (this is the scenario for, e.g., B[e] and Be stars). In symbotics, it would be interesting to watch the line profiles change during pulsation cycles for those systems that harbor a Mira, such as R Aqr, to see if individual absorption components are intercepted

by the line of sight to the WD. This requires con-tinual observations and times when the pathlength through the Mira wind is long, but it would be in-teresting to try. For AGB stars, we know the shells are ejected over timescales of the thermal pulses, you know this from the shells in planetary nebulae.

Coda

This is just the start of the discussion. The next column will be more specific on how you analyze such profiles, how to diagnose the driving and re-sponse conditions of the medium, and some sug-gestions of target objects. For those who have had the stamina to reach this point, and I hope the text hasn't been confusing, my thanks and warmest wishes for your observing success. Please write or scream, whatever seems appropriate, if there's anything you'd like to suggest or ask or critique. And my perpetual thanks to Francois for his pa-tience and comments. See you soon.

Steve Shore, 17-02-2019


Discovery of a Hot Symbiotic Star in the Cold Antarctic Sky: Symbiotics Are Outliers in SkyMapper uvgriz PhotometryAdrian B. Lucy1, J. L. Sokoloski, N. E. Nuñez, C. Wolf T. Bohlsen, and G. J. M. Lunahttp://iopscience.iop.org/article/10.3847/2515-5172/aaf71c/meta

... we report that Hen 3-1768 (≡ASAS J195948–8252.7) is a symbiotic star. ... Hen 3-1768 produced unambiguous emission from Raman O vi 6830,7088 Å, He ii 4686 Å, and other transitions, proving that it is a symbiotic star (e.g., Shore et al. 2014). Comparing to Pickles (1998) template spectra, we preliminarily con-strained the giant donor's spectral type to between K4 and K7, making Hen 3-1768 one of the dozen or so yellow symbiotics [...]

See also:- http://www.astrosurf.com/aras/Aras_DataBase/Symbiotics/Hen3-1768.htm- Hen3-1768- New symbiotics campaign

Disc instabilities and nova eruptions in symbiotic systems: RS Ophiuchi and Z AndromedaeBollimpalli, D. A.; Hameury, J. -M.; Lasota, J. -P.Monthly Notices of the Royal Astronomical Society, Volume 481, Issue 4, p.5422-5435

SUsing the disc instability model for dwarf novae and soft X-ray transients, we investigate the stability of accretion discs in long-period binary systems. We simulate outbursts resulting from this thermal-viscous instability for two symbiotic systems, RS Ophiuchi and Z Andromedae. The outburst properties deduced from our simulations suggest that, although the recurrent nova events observed in RS Oph are caused by thermonuclear runaway at the white dwarf surface, these run-aways are triggered by accretion disc instabilities. In quiescence, the disc builds up its mass, and it is only during the disc-instability outburst that mass is accreted on to the white dwarf at rates comparable to or larger than the mass-transfer rate. For a mass-transfer rate in the range 10-8 to 10^{-7} M_{☉} yr-1, the accretion rate and the mass accreted are sufficient to lead to a thermonuclear runaway during one of a series of a few dwarf nova outbursts, which are barely visible in the optical but easily detectable in the X-rays. In the case of Z And, persistent irradiation of the disc by the very hot white dwarf surface strongly modifies the dwarf nova outburst properties, making them significant only for very high mass-transfer rates, of the order of 10^{-6} M_{☉} yr-1, much higher than the expected secular mean in this system. It is thus likely that the so-called `combination nova' outburst observed in the years 2000 to 2002 was triggered not by a dwarf-nova instability but by a mass-transfer enhancement from the giant companion, leading to an increase in nuclear burning at the accreting white dwarf surface.https://arxiv.org/pdf/1804.07916.pdf

Dramatic change in the boundary layer in the symbiotic recurrent nova T Coronae BorealisLuna, G. J. M.; Mukai, K.; Sokoloski, J. L.; Nelson, T.; Kuin, P.; Segreto, A.; Cusumano, G.; Jaque Arancibia, M.; Nuñez, N. E. Astronomy & Astrophysics, Volume 619, id.A61, 7 pp.

A sudden increase in the rate at which material reaches the most internal part of an accretion disk, i.e., the boundary layer, can change its structure dramatically. We have witnessed such a change for the first time in the symbiotic recurrent nova T CrB. Our analysis of XMM-Newton, Swift Burst Alert Telescope (BAT)/X-Ray Telescope (XRT)/UltraViolet Optical Telescope (UVOT), and the American Association of Variable Stars Observers (AAVSO) V- and B-band data indicates that during an optical brightening event that started in early 2014 (∆V ≈ 1.5) the following occurred: (i) the hard X-ray emission as seen with BAT almost vanished; (ii) the XRT X-ray flux decreased significantly, while the optical flux remained high; (iii) the UV flux increased by at least a factor of 40 over the quiescent value; and (iv) the X-ray spectrum became much softer and a bright, new blackbody-like component appeared. We suggest that the optical brightening event, which could be a similar event to that observed about 8 years before the most recent thermonuclear outburst in 1946, is due to a disk instability.

X-ray, UV, and optical observations of the accretion disk and boundary layer in the symbiotic star RT CrucisLuna, G. J. M.; Mukai, K.; Sokoloski, J. L.; Lucy, A. B.; Cusumano, G.; Segreto, A.; Arancibia, M. Jaque; Nuñez, N. E.; Puebla, R. E.; Nelson, T.; Walter, F.Astronomy & Astrophysics, Volume 616, id.A53, 12 pp. (A&A Homepage)Compared to mass transfer in cataclysmic variables, the nature of accretion in symbiotic binaries in which red giants transfer material to white dwarfs (WDs) has been difficult to uncover. The accretion flows in a symbiotic binary are most clearly observable, however, when there is no quasi-steady shell burning on the WD to hide them. RT Cru is the prototype of such non-burning symbiotics, with its hard (δ-type) X-ray emission providing a view of its innermost accretion structures. In the past 20 yr, RT Cru has experienced two similar optical brightening events, separated by 4000 days and with amplitudes of ΔV 1.5 mag. After Swift became operative, the Burst Alert Telescope (BAT) detector revealed a hard X-ray brightening event almost in coincidence with the second optical peak. Spectral and timing analyses of multi-wavelength observations that we describe here, from NuSTAR, Suzaku, Swift/X-Ray Telescope (XRT) + BAT + UltraViolet Optical Telescope (UVOT) (photometry) and optical photometry and spectroscopy, indicate that accretion proceeds through a disk that reaches down to the WD surface. The scenario in which a massive, magnetic WD accretes from a magnetically truncated accretion disk is not supported. For example, none of our data show the minute-time-scale periodic modula-tions (with tight upper limits from X-ray data) expected from a spinning, magnetic WD. Moreover, the similarity of the UV and X-ray fluxes, as well as the approximate constancy of the hardness ratio within the BAT band, indicate that the boundary layer of the accretion disk remained optically thin to its own radiation throughout the brightening event, during which the rate of accretion onto the WD increased to 6.7 × 10-9M☉ yr-1 (d/2 kpc)2. For the first time from a WD symbiotic, the NuSTAR spectrum showed a Compton reflection hump at E > 10 keV, due to hard X-rays from the boundary layer reflecting off of the surface of the WD; the reflection ampli-tude was 0.77 ± 0.21. The best fit spectral model, including reflection, gave a maximum post-shock temperature of kT = 53 ± 4 keV, which implies a WD mass of 1.25 ± 0.02 M☉. Although the long-term optical variability in RT Cru is reminiscent of dwarf-novae-type outbursts, the hard X-ray behavior does not correspond to that observed in well-known dwarf nova. An alternative explanation for the brightening events could be that they are due to an enhancement of the accretion rate as the WD travels through the red giant wind in a wide orbit, with a period of about 4000 days. In either case, the constancy of the hard X-ray spectrum while the accretion rate rose suggests that the accretion-rate threshold between a mostly optically thin and thick boundary layer, in this object, may be higher than previously thought.

Recent publications

Symbiotics


Recent publications

Symbiotics


Broad absorption line symbiotic stars: highly ionized species in the fast outflow from MWC 560Lucy, Adrian B.; Knigge, Christian; Sokoloski, J. L.Monthly Notices of the Royal Astronomical Society, Volume 478, Issue 1, p.568-574

In symbiotic binaries, jets and disc winds may be integral to the physics of accretion on to white dwarfs from cool giants. The persistent out-flow from symbiotic star MWC 560 (≡V694 Mon) is known to manifest as broad absorption lines (BALs), most prominently at the Balmer transitions. We report the detection of high-ionization BALs from C IV, Si IV, N V, and He II in International Ultraviolet Explorer spectra ob-tained on 1990 April 29-30, when an optical outburst temporarily erased the obscuring `iron curtain' of absorption troughs from Fe II and similar ions. The C IV and Si IV BALs reached maximum radial velocities at least 1000 km s-1 higher than contemporaneous Mg II and He II BALs; the same behaviours occur in the winds of quasars and cataclysmic variables. An iron curtain lifts to unveil high-ionization BALs dur-ing the P Cygni phase observed in some novae, suggesting by analogy a temporary switch in MWC 560 from persistent outflow to discrete mass ejection. At least three more symbiotic stars exhibit broad absorption with blue edges faster than 1500 km s-1; high-ionization BALs have been reported in AS 304 (≡V4018 Sgr), while transient Balmer BALs have been reported in Z And and CH Cyg. These BAL-producing fast outflows can have wider opening angles than has been previously supposed. BAL symbiotics are short-time-scale laboratories for their giga-scale analogues, broad absorption line quasars (BALQSOs), which display a similarly wide range of ionization states in their winds.

Spectroscopic diagnostics of dust formation and evolution in classical nova ejecta

Shore, Steven N.; Kuin, N. Paul; Mason, Elena; De Gennaro Aquino, Ivanhttp://adsabs.harvard.edu/abs/2018arXiv180707174SIt has recently been discovered that some, if not all, classical novae emit GeV gamma rays during outburst, but the mechanisms involved in the A fraction of classical novae form dust during the early stages of their outbursts. The classical CO nova V5668 Sgr (Nova Sgr. 2015b) underwent a deep photometric minimum about 100 days after outburst that was covered across the spectrum. A similar event was observed for an earlier CO nova, V705 Cas (Nova Cas 1993) and a less optically significant event for the more recent CO nova V339 Del (Nova Del 2013). This study pro-vides a "compare and contrast" of these events to better understand the very dynamical event of dust formation. We show the effect of dust formation on multiwavelength high resolution line profiles in the interval 1200\AA\ - 9200\AA\ using a biconical ballistic structure that has been applied in our previous studies of the ejecta. We find that both V5668 Sgr and V339 Del can be modeled using a grey opacity for the dust, indi-cating fairly large grains (at least 0.1 micron) and that the persistent asymmetries of the line profiles in late time spectra, up to 650 days after the event for V5668 Sgr and 866 days for V339 Del, point to the survival of the dust well into the transparent, nebular stage of the ejecta evolu-tion. This is a general method for assessing the properties of dust forming novae well after the infrared is completely transparent in the ejecta.

V1369 Cen High-resolution Panchromatic Late Nebular Spectra in the Context of a Unified Picture for Nova Ejecta

Mason, Elena; Shore, Steven N.; De Gennaro Aquino, Ivan; Izzo, Luca; Page, Kim; Schwarz, Greg J.http://adsabs.harvard.edu/abs/2018ApJ...853...27MNova Cen 2013 (V1369 Cen) is the fourth bright nova observed panchromatically through high-resolution UV+optical multiepoch spectros-copy. It is also the nova with the richest set of spectra (in terms of both data quality and number of epochs) thanks to its exceptional bright-ness. Here, we use the late nebular spectra taken between day ~250 and day ~837 after outburst to derive the physical, geometrical, and kine-matical properties of the nova. We com pare the results with those determined for the other panchromatic studies in this series: T Pyx, V339 Del (nova Del 2013), and V959 Mon (nova Mon 2012). From this we conclude that in all these novae the ejecta geometry and phenomenology can be consistently explained by clumpy gas expelled during a single, brief ejection episode and in ballistic expansion, and not by a wind. For V1369 Cen the ejecta mass (~1 × 10-4 Mꙩ and filling factor (0.1 ≤ f ≤ 0.2) are consistent with those of classical novae but larger (by at least an order of magnitude) than those of T Pyx and the recurrent novae. V1369 Cen has an anomalously high (relative to solar) N/C ratio that is be-yond the range currently predicted for a CO nova, and the Ne emission line strengths are dissimilar to those of typical ONe or CO white dwarfs.

Recent publications

Novae

Eruptive stars spectroscopyCataclysmics, Symbiotics, Novae

cataclysmics, symbiotics, novae - astrosurf · aras eruptive stars information letter #40 2018-04 -...

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