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Observational Signatures of Planets Around the Black Hole at theMilky Way Center (SgrA*) Proto-Planetary Disk as the Source of the G2 Gas Cloud Hypervelocity planets and planets around hypervelocity stars
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Observational Signatures of Planets Around the Black Hole at theMilky Way Center ( SgrA *)

Feb 24, 2016

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Observational Signatures of Planets Around the Black Hole at theMilky Way Center ( SgrA *). Proto-Planetary Disk as the Source of the G2 Gas Cloud Hypervelocity planets and planets around hypervelocity stars. Stellar Orbits Around SgrA*. (BH at rest in GC). - PowerPoint PPT Presentation
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Page 1: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)

Observational Signatures of Planets Around the Black Hole at theMilky Way Center (SgrA*)

• Proto-Planetary Disk as the Source of the G2 Gas Cloud

• Hypervelocity planets and planets around hypervelocity stars

Page 2: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)

Stellar Orbits Around SgrA*

Ghez et al. 2008; Genzel et al. 2008

MBH = (4:5æ0:4) â 106M ì

dGC =8:4æ0:4kpc (BH at rest in GC)

Page 3: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)

Gillessen et al., Nature (2012)

*Ionized cloud, ~3x10^5 cm^{-3}, ~100AU, electrons at 10^4K, dust at 550K, 3 Earth masses

Page 4: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)

Latest Data

Gillessen et al. , submitted (2012)

Page 5: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)
Page 6: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)

Br-gamma slit

SgrA*

Page 7: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)

Br-gamma

Page 8: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)
Page 9: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)

Burkert et al. (2012)

Page 10: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)

Schartmann et al. (2012)

“Pressure-Confined Cloud” Model

Page 11: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)

Problem: why is the head moving on a ballistic orbit with no evidence for

ambient ram-pressure?

Page 12: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)

Tidal Disruption of a Proto-Planetary Disk Around a Low-Mass Star

Murray-Clay & Loeb (2012)

*Planets form near SgrA*

*Flags low-mass stars

Page 13: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)

Physical Parameters• Low-mass star, born in circum-nuclear ring at

~0.04pc, and scattered into orbit a few Myrs ago.

Original Current

Page 14: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)

• Low probability for scattering if this represents the first passage, but high probability for multiple passages in which the gas cloud is rejuvinated every pericenter passage (from ~1AU).

• Ionizing background from surrounding O-stars generates a ~10 km/s outflow from tidally-truncated disk of 1-10AU around M-dwarf (too faint to be observable).

• Photoevaporation yields a wind mass loss rate:

Page 15: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)

ionized

observed now

Br-pericenter

HI

observed

Page 16: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)

Hypervelocity Planets from Tidal Disruption of Stellar Binaries by SgrA*

Ginsburg, Loeb, & Wegner (2012)

Page 17: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)

Possible Outcome: Free Hypervelocity Planets

Page 18: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)

2 planets0.02 AU

4 planets0.02 AU 0.03AU

Probabilities of Outcomes

Page 19: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)

Transits of Hypervelocity Stars

Page 20: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)

Tidal Flares from Disrupted Planets or Asteroids

Waste dump: source of clean energy for galacto-centeric civilizations

Page 21: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)

Tidal Distruption of a Bound Object (e=0.8,beta=5)

Hayasaki, Stone, and Loeb 2012

Page 22: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)

Summary:

1. Evaporation of proto-planetary disks may flag low-mass stars at the Galactic Center.

2. Close-in planets around hypervelocity stars may cause detectable transit signatures.

Page 23: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)
Page 24: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)

Initial Ring Results in Two Bright Spots

Page 25: Observational Signatures of Planets Around the Black Hole at  theMilky  Way Center  ( SgrA *)

A Relativistic Jet from a TDE: Swift 164449.3+573451 (GRB110328A)

*Synchrotron and X-ray peaks are emitted from different regions; bulk Lorentz factor~2-3

Bloom et al. 2011 Zauderer et al. 2011