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Weiße Zwerge II Mikrolensing & Massenverteilung
Max Camenzind - Akademie HD - Sept. 2017
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Unsere Themen
• 40 Eridani B, Procyon B
• Mikrolensing an Stein 2051 B
• Was ist Mikrolensing?
• Spektralklassen für Weiße Zwerge
• Massen der Weißen Zwerge in der
Milchstraße
• Was ist die typische Masse eines WZ?
• Kühle Weiße Zwerge – wie kühl?
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WZ in 40 Eridani: A K1-Stern; B DA-WZ
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Das System 40 Eridani / StarObserver
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Procyon B:
Temperatur: 7740 K
M = 0,60 MS, R = 8600 km
r = 4,5 x 105 g/cm³
Alter ~ 2 Mrd. a
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1,0 MS
0,6 MS 0,4 MS
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Bond et al. 2015 Periode: 41 Jahre MA = 1,48; MB = 0,59 MS
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This Hubble Space Telescope image shows the binary star system Stein 2051 on October 1, 2013, consisting of the brighter, redder "A" component at lower right and the fainter, bluer "B" component near the center, a white dwarf star. Because these stars are relatively close to Earth, only 17 light-years away, they appear to move in the sky relative to the much more distant background stars in several months of observations with Hubble (he wavy blue line).
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Sucherkarte Stein 2051 Chamäleon
Grafik: Stellarium
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WFC3/HST
Image
Stein 2051
mit
Hinter-
grund-
sternen
für
Astro-
metrie [Sahu et al.]
Stein 2051 A
Stein 2051 B
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Sahu et al., arXiv:1706.02037
Parallaxenbewegung
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Lichtablenkung am Weißen Zwerg
Stein 2051 B mit HST / d = 17 LJ
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Linsen-Gleichung
Quellen-Ebene Linsen-Ebene
Beobachter
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Linsen-Gleichung
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Mikrolensing durch Punktquelle
qE qE = 31 mas p = 181mas DL = 5,52 pc
MB = 0,67 MS
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Video: Mikrolensing an Stein 2051 B
Der Weiße Zwerg Stein 2051B und ein ferner Hintergrundstern, aufgenommen vom Weltraumteleskop Hubble. (Credit: NASA, ESA, and K. Sahu (STScI))
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Spektroskopische Klassifikation
DA - nur Balmer Linien; kein HeI oder Metalle (75% der WZ)
DB – HeI Linien, kein H oder Metalle
DC – Continuum Spektrum, keine Linien tiefer als 5%
DO – starke HeII, HeI oder H-Linien im Spektrum
DZ – nur Metall-Linien, kein H oder He
DQ – Starkes Kohlenstoff-Feature
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Spektraltyp Weiße Zwerge mit Hipparcos
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Typische DA Weiße Zwerge
Hb Hg
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Spektrum: Weißer Zwerg Eridanus B
Maximum im Optischen Teff = 16.000 K ~ A
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Spektrum: Weißer Zwerg Sirius B
Barstow et al. 2005 Maximum im UV Teff = 25.000 K ~ B
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Spektrum: Weißer Zwerg Sirius B
Barstow et al. 2005
Hb
Hg
Hd
He
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Barstow et al. 2005
Parameter: Weißer Zwerg Sirius B
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Raddi et al. 2017 arXiv:1708.09394
Spektren
DA
Weiße
Zwerge Sortiert
nach
Temperatur
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Raddi et al. 2017 arXiv:1708.09394
Spektrum Weißer Zwerge
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Massenbestimmung Feldsterne
• Spektroskopische Methode:
Linienbreiten (Wasserstoff) hängen vom Druck ab proportional zu Gravitation + Masse-Radius Relation
g = GM/R2 Masse M
• Photometrische Methode:
Breitband Photometrie fitted an Black Body Teff und Winkeldurchmesser
Kombiniert mit Parallaxe Radius R
Verwende Masse-Radius Relation
Masse M
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In 2
0 p
c
12
9 W
eiß
e Z
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rge
D
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te =
0,0
033
MS/p
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Massenverteilung WZ innerhalb 40 pc
Dufour et al. 2016
nWZ = 0,0048 / pc³ In einer Kugel von 10 pc Radius 20 WZ
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1864 Weiße Zwerge mit m < 17 mag
Raddi et al. 2017; arXiv:1708.09394
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arXiv:1603.06666
Anfangs- & End-Massen von massearmen Sternen
Theorie
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SDSS mit Apache Point Telescope
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Apache Point Telescope Camera
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WZ SDSS Spektrum
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Massenhistogramm Weiße Zwerge Der typische WZ hat ~ 0,6 Sonnenmassen
SDSS DR4
1833 WZ
Madej et al. 2004
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SDSS DR7
19.712 WZ
Kleinman et al. 2012
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Kühle Weiße Zwerge mit Gemini
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Alte Weiße Zwerge mit HST