Similarities in the structureof the circumstellar environments

of B[e] supergiants and yellow hypergiants

Anna Aret1

Indrek Kolka1, Michaela Kraus1,2, Grigoris Maravelias2

1Tartu Observatory, Estonia2Astronomical Institute AV CR, Czech Republic

Spectroscopic survey of emission-line stars

1. GoalExplore the frequency and origin of [Ca II] and [O I] lines andstudy physical conditions traced by these lines

2. ObjectsEmission-line stars surrounded by dense circumstellar material

3. InstrumentCoude spectrograph @ Ondrejov 2 m telescope, Czech Republic:. H α: 6250–6760 A – R'13 000 (H α + [O I] λλ6300, 6364). [Ca II]: 6990–7500 A – R'15 000 ([Ca II] λλ7291, 7324). IR: 8470–8980 A – R'18 000 (Ca II λλ8498, 8542, 8662)

2 of 15Anna Aret (Tartu Observatory)

Survey: overview of the results

Sample of 58 objects:9 B[e] stars?, 4 YHGs, 1 post-AGB star, 2 peculiar objects with dense disks,30 Be stars, 3 emission-line stars of O–B types,9 pre-main-sequence stars (Herbig, T Tau, FU Ori).

Class [O I] [Ca II]B[e]SG + +low-mass B[e] + –YHG +/– +post-AGB + +peculiar +/– +Be – –O–B em – –pre-MS B[e] + +/–

?Aret et al. 2016, MNRAS 456, 1424

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Survey: B[e] supergiants V1478 Cyg and 3 PupMWC 349A HD 62623

[OI]

[OI]

Hα

[CaII]

[CaII]

CaII

Pa16

CaII

Pa15

Pa14

CaII

Pa13

Norm

alize

dflux

1.00

2.00

3.00

4.00

5.00

6300 6320 6340 6360 6380

50

100

150

200

250

300

6560 6580

1.00

1.10

1.20

1.30

1.40

1.50

7280 7300 7320 7340

1.0

2.0

3.0

4.0

5.0

6.0

8480 8500 8520 8540 8560 8580 8600 8620 8640 8660 8680

0.95

1.00

1.05

1.10

6300 6320 6340 6360 6380

1.0

1.2

1.4

1.6

1.8

2.0

2.2

2.4

2.6

6560 6580

0.80

0.90

1.00

1.10

1.20

1.30

7280 7300 7320 7340

0.4

0.6

0.8

1.0

1.2

1.4

1.6

1.8

8480 8500 8520 8540 8560 8580 8600 8620 8640 8660 8680

Wavelength (A)

V1478 Cyg

3 Pup

[OI] λλ6300,6364 Hα [Ca II] λλ7291,7324 Ca II IR λλ8498,8542,8662

4 of 15Anna Aret (Tartu Observatory)

Survey: B[e] supergiants V1478 Cyg and 3 PupKinematics obtained from the [O I] and [Ca II] line profiles agrees with anorigin of the lines in the Keplerian rotating rings

0.0

0.2

0.4

0.6

0.8

1.0

−100 −50 0 50 100

V1478 Cyg

[CaII]7324 Å

0.0

0.2

0.4

0.6

0.8

1.0

−100 −50 0 50 100

3 Pup

[CaII]7324 Å

0.0

0.2

0.4

0.6

0.8

1.0

−100 −50 0 50 100

OY Gem

[CaII]7324 Å

0.0

0.2

0.4

0.6

0.8

1.0

−100 −50 0 50 100

V1429 Aql

[CaII]7324 Å

0.0

0.2

0.4

0.6

0.8

1.0

−100 −50 0 50 100

V1478 Cyg

[OI]6300 Å

0.0

0.2

0.4

0.6

0.8

1.0

−100 −50 0 50 100

3 Pup

[OI]6300 Å

0.0

0.2

0.4

0.6

0.8

1.0

−100 −50 0 50 100

OY Gem

[OI]6300 Å

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Survey: B[e]SG vs YHG

Object Sp.type [O I] [Ca II] Ca II IR

V1478 Cyg MWC 349A B0-B1.5 I + + emis3 Pup HD 62623 A2.7 Ib + + emis

V1302 Aql IRC +10420 A2-F8Ia + + emisV509 Cas HR 8752 A7-G5Ia + + emis/absρ Cas HD 224014 F0-G7Ia – + absV1427 Aql HD 179821 F3-G5Ia – + abs

6 of 15Anna Aret (Tartu Observatory)

B[e]SG

YHG

B[e]SG 3 Pup vs hot YHGs V1302 Aql & V509 Cas[O

I]

[OI]

Hα

[CaII]

[CaII]

CaII

Pa16

CaII

Pa15

Pa14

CaII

Pa13

Norm

alize

dflux

0.95

1.00

1.05

1.10

6300 6320 6340 6360 6380

1.0

1.2

1.4

1.6

1.8

2.0

2.2

2.4

2.6

6560 6580

0.80

0.90

1.00

1.10

1.20

1.30

7280 7300 7320 7340

0.4

0.6

0.8

1.0

1.2

1.4

1.6

1.8

8480 8500 8520 8540 8560 8580 8600 8620 8640 8660 8680

0.90

0.95

1.00

1.05

1.10

1.15

6300 6320 6340 6360 6380

1.0

2.0

3.0

4.0

5.0

6.0

7.0

6560 6580

1.00

1.40

1.80

2.20

2.60

7280 7300 7320 7340

1.0

1.5

2.0

2.5

3.0

8480 8500 8520 8540 8560 8580 8600 8620 8640 8660 8680

0.94

0.96

0.98

1.00

1.02

1.04

6300 6320 6340 6360 6380

0.8

1.0

1.2

1.4

1.6

1.8

6560 6580

0.90

0.95

1.00

1.05

1.10

1.15

1.20

1.25

7280 7300 7320 7340

0.2

0.4

0.6

0.8

1.0

1.2

8480 8500 8520 8540 8560 8580 8600 8620 8640 8660 8680

Wavelength (A)

3 Pup

V1302 Aql

V509 Cas

[OI] λλ6300,6364 Hα [Ca II] λλ7291,7324 Ca II IR λλ8498,8542,86627 of 15

Anna Aret (Tartu Observatory)

B[e]SG 3 Pup vs cool YHGs V1302 Aql & V509 Cas[O

I]

[OI]

Hα

[CaII]

[CaII]

CaII

Pa16

CaII

Pa15

Pa14

CaII

Pa13

Norm

alize

dflux

0.95

1.00

1.05

1.10

6300 6320 6340 6360 6380

1.0

1.2

1.4

1.6

1.8

2.0

2.2

2.4

2.6

6560 6580

0.80

0.90

1.00

1.10

1.20

1.30

7280 7300 7320 7340

0.4

0.6

0.8

1.0

1.2

1.4

1.6

1.8

8480 8500 8520 8540 8560 8580 8600 8620 8640 8660 8680

0.6

0.7

0.7

0.8

0.8

0.9

0.9

1.0

1.0

6300 6320 6340 6360 6380

0.5

0.6

0.7

0.8

0.9

1

1.1

6560 6580

0.85

0.90

0.95

1.00

1.05

1.10

7280 7300 7320 7340

0.2

0.3

0.4

0.5

0.6

0.7

0.8

0.9

1.0

8480 8500 8520 8540 8560 8580 8600 8620 8640 8660 8680

0.5

0.6

0.7

0.8

0.9

1.0

6300 6320 6340 6360 6380

0.5

0.6

0.7

0.8

0.9

1

6560 6580

0.80

0.85

0.90

0.95

1.00

1.05

1.10

1.15

7280 7300 7320 7340

0.2

0.4

0.6

0.8

1.0

8480 8500 8520 8540 8560 8580 8600 8620 8640 8660 8680

Wavelength (A)

3 Pup

ρ Cas

V1427 Aql

[OI] λλ6300,6364 Hα [Ca II] λλ7291,7324 Ca II IR λλ8498,8542,86628 of 15

Anna Aret (Tartu Observatory)

General similarities (Galactic & extragalactic objects)

B[e]SG YHG

[Ca II] all all[O I] all hotterCO band most most

(variability) (some) (all)IR excess / dust all manyCMS structure disca/ringb discc/shellMass loss mechanism pulsations?d pulsationse

ae.g. Leinert 1986; Millour et al. 2011; bMaravelias et al. this conference; cOudmaijer & de Wit 2013

dV743 Mon: Borges Fernandes et al. 2012; LHA 120-S 73: Kraus et al. 2016; eoverview by de Jager (1998)

Zickgraf (1998): Is V1302 Aql a pre-B[e] supergiant?

9 of 15Anna Aret (Tartu Observatory)

Evolutionary connection

4.6

4.8

5

5.2

5.4

5.6

5.8

6

3.43.63.844.24.44.64.8

log

L/L O•

log Teff

B[e]SGYHG

V1302 Aql

ρ CasV509 CasV382 Car

V1427 Aql

10 of 15Anna Aret (Tartu Observatory)

Evolutionary connection

4.6

4.8

5

5.2

5.4

5.6

5.8

6

3.43.63.844.24.44.64.8

log

L/L O•

log Teff

25M

O•20M

O•

32MO•

40MO•

B[e]SGYHG

V1302 Aql

ρ CasV509 CasV382 Car

V1427 Aql

Ekström et al. 2012

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Evolutionary connection

4.6

4.8

5

5.2

5.4

5.6

5.8

6

3.43.63.844.24.44.64.8

log

L/L O•

log Teff

25M

O•20M

O•

32MO•

40MO•

B[e]SGYHG

V1302 Aql

ρ CasV509 CasV382 Car

V1427 Aql

Ekström et al. 2012Nieuwenhuijzen et al. 2012

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Evolutionary connection

4.6

4.8

5

5.2

5.4

5.6

5.8

6

3.43.63.844.24.44.64.8

log

L/L O•

log Teff

25M

O•20M

O•

32MO•

40MO•

B[e]SGYHG

V1302 Aql

ρ CasV509 CasV382 Car

V1427 Aql

Ekström et al. 2012Nieuwenhuijzen et al. 2012

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YHGs: bluewards evolution across the HRD

V1302 Aql – F81 =⇒ A22: increase in Teff ∼ 120 K/yr in 1973–2002Klochkova et al. 2016: Teff does not increase any further

V509 Cas – Nieuwenhuijzen et al. 2012: Fast growth of Teff in 1973–2005Sheet1

Page 1

40000 42000 44000 46000 48000 50000 52000 54000 56000 58000 600004000

5000

6000

7000

8000

9000V509 Cas

Julian day - 2 400 000

Effe

ctiv

e te

mpe

ratu

re

Aug 1973

Nov 2015

March 2001

1Humphreys et al. 1973; 2Klochkova et al. 200214 of 15

Anna Aret (Tartu Observatory)

Ondrejov↖

Conclusions

1. Forbidden lines of [O I] and [Ca II] provide an ideal tool toidentify objects with similar circumstellar environments

2. Appearance of [Ca II] lines requires environments of highdensity and large emitting volume

3. Both sets of lines are detected in B[e]SGs and hot YHGs,Ca II IR triplet is in emission

4. [Ca II] are detected also in cool YHGs,Ca II IR triplet is in absorption

5. Fast heating of V509 Cas has slowed down

Similarities between B[e]SGs and YHGs indicatepossible evolutionary connection

15 of 15Anna Aret (Tartu Observatory)