symbio/c x-ray binaries - gemini observatory · 2018-08-02 · and a hot, compact, usually a white...

CosmicSurvivors:Symbio/cX-rayBinaries

K.Hinkle,R.Joyce,V.Smith(NOAO)F.Fekel(TennState)

J.Mikolajewska,C.Galan(CopernicusInst.)T.Lebzelter(Vienna)

Symbio/cX-rayBinaries

K.Hinkle,R.Joyce,V.Smith(NOAO)F.Fekel(TennState)J.Mikolajewska,C.Galan(CopernicusInst.)T.Lebzelter(Vienna)

Outline

1.  Symbio/cbinaries,thegood,bad,andugly2.  A“typical”S-symbio/c

3.  Neutronstarsymbio/cbinaries=SyXB

4.  SyXBbinaryevolu/on

Symbio/cStars–SyStdefinedbyop/calspectrathatcombinehighenergy

emissionlines+latetypegiantfeatures

Allen1984ApSS99101

FurtherDividedintoSandDtypes

S-typeslackstrongIRexcess D(dusty)-typesaremiras

Modernunderstandingofsymbio/cstars

Oneofafamilyofbinariesconsis/ngofalate-typestarandahot,compact,usuallyawhitedwarf,companion

SyStclass(normalsymbio/cbinaries)definedby:• Masstransfer

-Generatesemissionlinespectrum-Rochelobeflowtoaccre/ondisk

• RedGiant/AGB+degenerate- S-type:NormalMIII,orbitsoffewyears- D-type:Mira,orbitsofdecades

Emissionlines–UV/Op/calproblem

Op/calSpectrum4600–5050Å

St2-22-Tomovetal.2017ActaAstronomica67225

IRspectrum2.0–2.5µmSt2-22-Tomovetal.2017ActaAstronomica67225

IRspectra&dataproducts

•  Orbits–  Timeseriesofspectraspanningyearstodecades

–  Difficulttogettheobserva/ons.TACslikeshorttermgoals.

–  IRVelocitydata:KimPeak(coudefeed,2.1m,4m),MtStromlo1.9m,Fairborn2m,GeminiSouth

–  30+orbits,Fekel,Hinkle,Joyce,etal.•  Abundances

–  IRabundancedata–highresolu/on,highS/N,keyspectralfeatures

–  KPNO4m/Phoenix&GeminiSouth/Phoenix/IGRINS

–  20+stars,Gałan,Mikołajewska,Hinkle,etal.

SySt=observedcharacteris/cnotuniqueevolu/onarystate

•  Mul/pleevolu/onarypathsconvergetoSySt

•  Eachsystemneedstobeunderstoodseparately

Part2

A“typical”Symbio/c

MIII+whitedwarf

∴Progenitormassesboth<8M!

CICyg:M5II+WDS-typeSymbio/cphotometry-WDeclipses

Eclipsingsymbio/csystemscommon

•  Radiusofredstarishugecomparedtowhitedwarf

•  Binaryeclipsecriteria:acosi<Rrg+Rwdwherea=semimajoraxisi=inclina/onR=stellarradius-  Rrglarge&semimajoraxistypicallylessthan10Rrg

" largerangeofithateclipses

#Dura/onoftheeclipseameasureofRrg

Fekeletal.2000AJ1191375

MIIIRadiusandMass

•  DistanceforGaiaandphotometry"L=2261L!

•  SpectraltypeM5III"Teff=3300K•  L=R2T4"R=145R!$

•  RedgiantnotRochelobefilling=“detached”•  Pulsa/onPeriod=50days"AGBfirstovertone•  Pulsa/ontheoryforAGBstars:logR=(logP+0.5logM+1.40)/1.5solveforM" 2M!

Orbitsolu/on:f(m)=0.0262Eclipsedura/on->i=73°

Mredgiant=2M!$

solveforWDmass:Mwhitedwarf=0.6M!

FromWDini/al–finalmassrela/onMSmasswas~2M!$

ProgenitorMSbinary-twosimilarlateAstars $

f(m)=(m3wdsin3i)/(mrg+mwd)2

Part3

Neutronstarsymbio/cbinaries=SyXB

MIII+neutronstar

Atleastonestarhad

aprogenitorM>8M!

Prototype(?)GX1+4=V2116Oph

•  Bright,hardX-raysource•  NSmagne/cfield~1013G•  X-ray&op/calpulsar– VerylongpulsarP~2minutes

– Varia/onsduetovariablemassaccre/onrate

Orbitalperiod3.18yrs

Hinkleetal.2006ApJ641479

NSmassknown(?)

•  MNS=1.35±0.04M!$

(atleastinHMXB)

Thorsem&Chakrabary1999

ApJ512288

MIIIRadius,Luminosity,&Mass

•  Massfunc/onlargebutnoeclipsessoi~70"MRG~1M!$

•  Usingstandardtricks, RRG=103R!

L=1270L!$

•  Soredgiantisat/pRGBorlowerAGB

Theremustbemorethanoneobservableneutronstarsymbio/c.Thereare50whitedwarf–neutronstarbinaries.

Illustra/on©G.Booth

8SyXBfoundinrecentsearches

•  SearchforMIIIatX-raycoordinates

•  ConfirmNSwithX-rayspectrum

•  Op/calemissionspectrumisweak!– V2116Ophistheexcep/on

Mase{etal.2006A&A,Lüetal.2012MNRAS

V934Her,Porb=12.0yrs

Hinkleetal.inprepara/on

Mass,etc.

•  GaiaD=544pc,Teff=3600K,L=1800L!,R=110R!,P1stovertone=44days,andtheusualtricks:

-MRG=1.2-1.5M!

-MNS=1.35M!

•  Solvefori"~11°"viewingnearlypoleon– Agreeswithnopulsardetec/on.

•  a=813R!sosystemisdetached

Abundances

•  ForV2116OphandV934HerwehaveIGRINSandPhoenixspectra

•  Measuredcarbonandoxygenisotopes

FirstdredgeupmodelsconnectMSmassto12C/13Cand16O/17O

Smith1990,MemSoc.Astron.Italiana61787FigurefromHinkleetal.2016ApJ82538

SummaryofSyXBsystems

•  MIIIprogenitorswere1.0–1.3M!stars•  MIIIcurrently:– ~1M!(V2116Oph)

– 1.2–1.5M!(V934Her)

•  MIIIshowsnoindica/onofeithersignificantmassaccre/onormassloss

Part4

SyXBevolu/on

•  Massivestarpassedthroughsupergiantstage–  Rsupergiant~800R!$

–  OverfillscurrentRochelobesize– ∴Orbitevolu/on

•  NSfromasupernova–  CCsupernova"kickvelocity?–  StrippedCCsupernova,lesskick,mechanism?

•  LowmassstarnowRGorearlyAGBstar– MirastagewillfillcurrentRochelobe

Constraints

CommonEnvelopePath

• MassivestarevolvestooverfullRochelobe

• CEstagereducesmassinsystem

• Nakedheliumstar"typeIb/csupernova• ProducesNSwithlowkickvelocity

PROBLEM–CEmasslossreducesorbitalperiodfromyearstodays

Willems&Kolb2002MNRAS3371004

CCSupernovapath

• NoRocheoverflowofevolvedmassivestar

• CoreCollapseSN• Survivesifkickissimilartoandinoppositedirec/onfromorbitalvelocity• ResultisMS+NSinlongperiodorbit

• MasstransferduringMirastagespinsupNSandexpandsRLsize

• EndproductisNS+WDlongperiodbinaryWillems&Kolb2002MNRAS3371004

WorkinProgress

•  Addi/onalSyXBorbitsunlikelyusingopenaccesstelescopes– Orbitsrequiredecadelong/meseriesofspectra

•  Abundanceworkinprogress–IGRINS–  MIIIprogenitormass

– Progenitorpopula/on– TracesofSN?

TheEnd