white dwarfs, planets, disks marc kuchner nasa goddard space flight center
DESCRIPTION
White Dwarfs, Planets, Disks Marc Kuchner NASA Goddard Space Flight Center Laboratory for Exoplanets and Stellar Astrophysics. Laboratory for Exoplanets and Stellar Astrophysics NASA Postdoctoral Program: http://nasa.orau.org/postdoc/ Exoplanet Talks: http://eud.gsfc.nasa.gov/ - PowerPoint PPT PresentationTRANSCRIPT
White Dwarfs, Planets, Disks
Marc Kuchner
NASA Goddard Space Flight Center
Laboratory for Exoplanetsand Stellar Astrophysics
Laboratory for Exoplanetsand Stellar Astrophysics
NASA Postdoctoral Program:http://nasa.orau.org/postdoc/
Exoplanet Talks: http://eud.gsfc.nasa.gov/ Marc.Kuchner/exoplanetclub.html
Spitzer Space Telescope
White DwarfBill Reach (IPAC)Ted von Hippel, Don Winget,Mukremin Kilic, Fergal Mullaly(UT Austin)Adam Burrows (U. Arizona)
Wavelength (microns)
White DwarfG29-38
Zuckerman &Becklin 1987
1200 K0.15 Rsun
~40 Jupitermassesby age and T
H
He
CMg
Fe
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log mass (solar masses)
Rad
ius
(Ear
th R
adii)
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White Dwarf
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log mass (solar masses)
Rad
ius
(Ear
th R
adii)
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G29-38b ?
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Jupiter
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DZ
75% 10% 5% 10%
Helium Surface
Hydrogen Surface
No Lines fromSurface!
DQ
DX
Metal, Carbon,Or Unidentified
Carbon andOxygen Core
DA DCDB
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~20% of DAs, including G29-38
Hydrogen Surface with Metals
DAZ
CO core
Teff (K)
Bergeron et al. 2004
DA InstabilityStrip
L
og g
615s
P
ower
23 JUL 1988B-band
24 JUL 1988K-band
Patterson et al. 1991
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Pulsation Timing
(Kleinman et al. 1998) & speckle photometry (Kuchner et al. 1998)
HST/Gemini Photometry
(Debes et al. 2005)
Debes et al. 2005
Log R (AU)
MJu
pite
r
Deuterium Burning Limit
e.g. Debes & Sigurdsson 2002, Jura et al. 2003
Spitzer Space Telescope
White Dwarf
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Jupiter at 5 microns w/ ISO (Encrenaz et al. 1997)
Typical WD ages since formation ofprogenitor are 1.5 - 3.5 109 years.
Planet mass (MJupiter)0 5 10 15
0.3
0.2
0.1
0.0Pla
net/W
D a
t 4.5
mic
rons
109 yr.
3 109 yr.
Spitzer photometry
CIA
Bergeron et al. 1994
Kilic et al. 2006, ApJ, in press
Same Modelsw/ CIA
New Spitzer Photometry
Without the mid IR data:
5400 K, 3.5 Gyr old.
With the mid IR data:
5200 K, 4.5 Gyr old
FJ/FV
F8
m/F
VDZ
All Hydrogen WDs below ~7000 Kshow an 8 micron deficit!
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Galactic Disk:8 +/- 1.5 Gyr
Von Hippel et al., in prep
A New Dusty WD!
Kilic et al. 2005Becklin et al. 2005
Becklin & Zuckerman 1987
Kilic et al., in prepGD 56
Plus 2 more from IRTF and one from Farihi et al makes 5!
Amorphous carbon needed tomatch 1.6 m spectrum
amorphousolivine
forsterite
Reach et al. 2005
C:O ratio 3:11-10RSun
0.01-1000 m grains dn/da a-3.5
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Livio, Pringle & Saffer 1992
H
He
CMg
Fe
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log mass (solar masses)
Rad
ius
(Ear
th R
adii)
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White Dwarf
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C:O ratio in gas 9:1 Roberge et al. in press
11.3 micron C-Hout-of-plane bend
T Tauri Stars -- Spitzer
Geers et al 2005
Particle Plieups Youdin & Chiang 2004
Lodders& Fegley 1997
Wood &Hashimoto1993
Atomic Fraction
SiC
Forsterite
Cohenite
EnstatiteFe
EnstatiteChondrites?
Gas and Graphite
Gaidos 2000Kuchner & Seager 2005
Artist: Lynette Cook
Solar Composition
Kuchner & Seager 2005
Carbon Planet
Kuchner & Seager 2005
Kuchner & Seager 2005
Kuchner & Seager 2005
Tim
e o
f A
rriv
al R
esid
ual
s (
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w/o planets
withnon-interactingplanets
with realplanets
Konacki & Wolzsczan 03
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Cool Hydrogen WDs have mid-IR deficits; the inferred age of theGalactic disk is wrong by ~25%.
Roughly 1/4 DAZ WDs are dusty.
The dust sometimes has silicates----but it may be C rich (e.g. G29-38).
Carbon planets may be common; we can recognize them if they are hot.
Key Points
New Exoplanet Lab at Goddard: come join us as a postdoc or asa speaker!
Wavelength (microns)
Flu
x (m
Jy)
A WD Planet With A Dust Disk
Reach, Von Hippel& Kuchner et al. 2005
Plus one more from Farihi et al. (private comminucation).
That makes 5 dusty DAZs out of 20 DAZs with 8 micronPhotometery.
DAZd ?
New Dusty WDs from IRTF:GD56+GD362(Kilic et al 2006)
GD362 also found byBecklin et al. 2006
The SunGalactic Center
Carigi et al. 2005
Dead Star:White DwarfG 29-38
Solar SystemDust
6 8 10 12 14
Wavelength (microns)
Rel
ativ
e br
ight
ness
Spitzer Sees Ghostof Solar System’sFuture
Marc KuchnerGoddard Space Flight Center
Bill ReachSpitzer Science Center
Ted von HippelUniversity of Texas, Austin
Oppenheimer et al. 2001
Bergeron & Leggett 2002
UltraCool WDs (<4000 K)