update on binary central stars (with an eye on...
TRANSCRIPT
![Page 1: Update on Binary central stars (with an eye on ChanPlaNS)urizen-physics.nsm.du.edu/~tueta/HerPlaNS/Site/Talks/Corradi.pdfUpdate on Binary central stars (with an eye on ChanPlaNS)](https://reader033.vdocument.in/reader033/viewer/2022041509/5e271351ff092e2be03cfe4f/html5/thumbnails/1.jpg)
Brent Miszalski (SAAO/SALT) Henri Boffin & Dave Jones (ESO),
Romano Corradi & Pablo Rodríguez-Gil (IAC),
Miguel Santander-García (OAN)
Update on Binary central stars
(with an eye on ChanPlaNS)
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How to find binaries
• Direct imaging: limited to wide systems. No P
determination, but >102 years.
• Light curves: irradiation, ellipsoidal variations (contact
or semi-detached binaries), eclipses. P≤ a few days
• Radial velocity curves. P≤ few102 days
• Spectroscopic or photometric detection of “cool” (=not
hot enough) companions. No P.
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Close binaries (firm)
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Single (?) stars Some objects probably just single stars with X-rays generated in
clumpy winds (e.g. NGC6543) - work by Guerrero/De Marco
• NGC4361:
• 3xSALT spectra --> no big shifts
• Flat SAAO lightcurve
Some others could be mergers
• IC4663: [WN3] CSPN, He-rich (95%) atmosphere (Miszalski+ 2012)
• (V)LTP scenarios CANNOT explain He-rich composition
• 3 epochs show no RV variability
• WD+WD merger best scenario (Reindl+ 2013; Miszalski+2013)
Would a WD+WD merger product show a (spun-up?) CSPN with X-ray
signature?
IC4663
Miszalski+2012
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Double degenerates
• A41 (Shimanskii et al. 2008)
• PN G135.9+55.9 (TS01, Tovmassian et al. 2010)
• V458Vul (Nova Vul 2007, Rodriguez et al. 2008)
• NGC6026 (Hillwig et al. 2010)
• Fg1 (Boffin et al. 2012)
• Hen 2-428 (Santander et al. 2013)
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Double degenerates
• TS01: Hot component Teff = 160–180 kK, a luminosity of about ∼104
L. Probably bloated and heated as a result of intense accretion and
nuclear burning on its surface in the past. Cool component has Teff =
60kK.
• Ellipsoidal variation + flickering accretion.Total mass of the binary
system is close to the Chandrasekhar limit SNIa candidate
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Fleming1 Boffin et al. 2012, Science, 338, 773
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Fleming1
VLT FORS
radial velocity
curve
Flat lightcurve
Boffin et al. 2012, Science, 338, 773
Need RV
monitoring to
find DDs!
long assumed binary
now proven!
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Envelope from shocked jets as
first predicted by Cliffe et al.
Raga+
2009
Cliffe+ 1995, 1996 Raga+ 2009 Boffin+ 2012
Fleming1: binary shaped jets
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Hen 2-428
Santander-García et al. , in preparation
dense circumstellar medium (ne=103.3-
6 cm-3) + zone with ne>1010 cm-3 (from
Ca II triplet in emission) accretion
disc?
P=4 hours, ellipsoidal variations
2 contact-WDs?
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V458 Vul: Nova Vul 2007
Wesson et al. 2008, ApJ 688, L21
Rodriguez-Gil et al. 2010, MNRAS 407, L21
P=98 min
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V458 Vul
A nova with such a short period MUST be an old system, MUCH
older than the 14000 yr old PN
the PN is the SECOND one of the system (after a 2nd common-
envelope stage)
2 WDs, M = 0.58M (photoionisation model) and M > 1M (nova
theory) Mtotal > 1.6 M > MChandrasekhar V458 Vul is another
SN Ia candidate
(GK Per (Nova Per 1901) might be another case of a nova inside a PN)
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Accretion in CSPN?
• Except for TS01, V458 Vul and possibly Hen 2-428, in
general we see no evidence for active accretion on the hot
central star in PNe. Almost all post-CE systems are
detached
• Therefore, it is possible some post-CE nuclei may emerge
from CE phase semi-detached/interacting at lower end of
period distribution
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Wind Accretion (on secondaries)
• Formation scenario: Polluted material accreted via wind
accretion (e.g. Wind RLOF) from WD progenitor during
its AGB phase
• Barium CSPN: S-process and carbon enriched
(sub)giants with evolved WD companions
• Carbon dwarfs: enriched by PN progenitors in their
carbon star AGB phase
• PNe provide the best evidence: as they catch the
systems right after the “main act”.
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Wind Accretion on secondaries
• Bona-fide barium CSPN: LoTr5, A70, WeBo1
• Accretion spins up red giant => Fast rotation velocity (near
break up) and...
• sometimes X-rays - LoTr 5 (Montez et al. 2010)
• Some ChanPlaNS detections suspected:
• NGC7008 and NGC6445 (need follow-up)
• Also happens in post-CE systems
• The Necklace (Miszalski, Boffin & Corradi 2013)
• Might explain „bloated‟ secondaries in post-CE systems
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White Dwarf
V~20.4 mag
GALEX
G8IV-V
V~17.8 mag
GMOS
SED Abell 70 Miszalski+ 2012
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WeBo 1 Bond+2003
WeBo1 WD
detected by
SWIFT/UVOT
Siegel+ 2012
(Not detected
in Swift X-ray
observations)
WeBo1 analogue found in South by SALT
(Miszalski+2013 to be submitted soon)
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The Necklace Corradi+ 2011
Miszalski, Boffin & Corradi 2013
Carbon dwarf + preWD
•Accretion BEFORE
CE phase C/O>1
•Consistent with jet
dynamic age (pre-PN)
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Jet formation in PNe
• In past, jets have mostly been studied in pre-PNe, but binary
status of pre-PNe poorly understood
• Several post-CE PNe are known to have jets
• Not highly collimated => precession influenced
• Most post-CE PNe have jets ejected before main nebula (CE)
• Thought to launch from accretion disk around companion PRIOR
to (very short) CE phase (e.g. Huarte-Espinosa+2013)
• Observational evidence only now available to demonstrate this is
the case for most systems. Necklace best example.
ETHOS1
Mis
zals
ki+
20
11
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(Romano‟s) summary Increasing evidence for post-CE binaries in CSPNe. Total fraction still
undetermined, but ≥20%
Clear relation between (CE) binarity and some morphological features,
mainly rings and jets. Mild (broad-waist) bipolars also frequently found.
But a variety of other morphologies also found.
Still no direct evidence for binarity in the most classical (narrow-waist)
bipolars like NGC6302, NGC6537, MyCn18, M2-9, Mz 3, etc. Long period
binaries? RV programme ongoing, results at APN6.
A lot of new evidence of pre-CE accretion onto secondaries barium stars,
carbon dwarfs. This is now assumed to be the cause of pre-CE jets.
Some systems (6 out of 40) double degenerates. Some are good SNIa
progenitors.
Binary CSPN with X-ray detection need dedicated study. For several of them,
little is known about the basic binary parameters.
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Thanks for listening!
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SALT HRS
Durham Centre for
Advanced
Instrumentation
• High Resolution Spectrograph to arrive mid-2013 at SALT -
ideal for relatively bright CSPN at δ<11.25°
• Fibre fed, temperature stabilized vacuum tank design
• Three modes: R=16 000, 37 000 and 65 000
• Wavelength range: 380-890 nm over two CCDs
• CHANPLANS sample: RV monitoring and high quality spectra
for model atmosphere fitting