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.

Slides:

Advertisements

Similar presentations

February 9, 11:00 am. The unusually bright centers found in some galaxies are called 1.active galactic nuclei. 2.starbursts. 3.halos. 4.supermassive.

Advertisements

Formation of Stars Physics 113 Goderya Chapter(s):11 Learning Outcomes:

ASTR100 (Spring 2008) Introduction to Astronomy The Milky Way Prof. D.C. Richardson Sections

14.2 Galactic Recycling Our Goals for Learning How does our galaxy recycle gas into stars? Where do stars tend to form in our galaxy?

A105 Stars and Galaxies  Milky Way Homework (#11) due today  Projects Due Nov. 30  For next week: Units 74, 75, 76, 78, 79  “rooftop” tonight, 8 PM,

COSPAR Workshop, Udaipur 2003 Active Galactic Nuclei : I Keith Arnaud NASA Goddard University of Maryland.

Jets from stellar tidal disruptions by supermassive black holes Dimitrios Giannios Princeton University HEPRO3, Barcelona, June 30.

Modeling the X-ray emission and QPO of Swift J Fayin Wang ( 王发印） Nanjing University, China Collaborators: K. S. Cheng (HKU), Z. G. Dai (NJU), Y.

Probing Dormant Massive Black Hole Binaries at Galactic Nuclei Fukun Liu Astronomy Department & KIAA, Peking University, Beijing, China Probing Strong.

Lecture Outline Chapter 15: Our Galaxy © 2015 Pearson Education, Inc.

What Are the Faint X-ray Transients Near the Galactic Center? Michael Muno (UCLA/Hubble Fellow) Fred Baganoff (MIT), Eric Pfahl (UVa), Niel Brandt, Gordon.

Galaxies with Active Nuclei Chapter 17. You can imagine galaxies rotating slowly and quietly making new stars as the eons pass, but the nuclei of some.

Fabio Antonini Joshua Faber Alessia Gualandris and David Merritt Rochester Institute of Technology.

The Swansong of Stars Orbiting Massive Black Holes Clovis Hopman Weizmann Institute of Science Israel Advisor: Tal Alexander.

Ge/Ay133 What (exo)-planetary science can be done with microlensing?

How Do Supermassive Black Holes Get Starved? Q. D. Wang, Z. Y. Li, S.-K. Tang University of Massachusetts B. Wakker University of Wisconsin.

Numerical Modeling of Electromagnetic Radiation from AGN Jets Based on  -ray emission and spectral evolution of pair plasmas in AGN jets Bottcher et al.

The general theory of relativity is our most accurate description of gravitation Published by Einstein in 1915, this is a theory of gravity A massive object.

Close encounters between stars and Massive Black Holes Clovis Hopman Weizmann Institute of Science Israel Advisor: Tal Alexander.

Multi-Messenger Astronomy of Tidal Stellar Pablo Laguna Center for Relativistic Astrophysics School of Physics Georgia Tech, Atlanta, USA Amaldi 11, Gwangju,

The Milky Way Center, Shape Globular cluster system

Our Galaxy The Milky Way. The Milky Way Almost everything we see in the night sky belongs to the Milky Way We see most of the Milky Way as a faint band.

The Milky Way Our Galaxy Please press “1” to test your transmitter.

Cosmic Rays Discovery of cosmic rays Local measurements Gamma-ray sky (and radio sky) Origin of cosmic rays.

The Milky Way and Other Galaxies Science A-36 12/4/2007.

Black Holes Monsters Lurking at the Centers of Galaxies

Star and Planet Formation Sommer term 2007 Henrik Beuther & Sebastian Wolf 16.4 Introduction (H.B. & S.W.) 23.4 Physical processes, heating and cooling.

J. Cuadra – Accretion of Stellar Winds in the Galactic Centre – IAU General Assembly – Prague – p. 1 Accretion of Stellar Winds in the Galactic Centre.

Stellar Disruptions of Super Massive Black Holes Ron Caplan March 7, 2003.

The Current Status of Hypervelocity Stars Galactic Center Workshop Shanghai 2009 Oct 21 Warren R. Brown Smithsonian – CfA Collaborators: Margaret Geller,

Active Galaxy Jets – An exhausting business Diana Worrall University of Bristol.

Case Western Reserve University May 19, Imaging Black Holes Testing theory of gas accretion:Testing theory of gas accretion: disks, jets Testing.

1 The Precision Radial Velocity Spectrometer Science Case.

Quasars, black holes and galaxy evolution Clive Tadhunter University of Sheffield 3C273.

Black Hole Chaos The Environments of the most supermassive black holes in the Universe Belinda Wilkes, Chandra X-ray Center, CfA Francesca Civano, CfA.

Star Formation in our Galaxy Dr Andrew Walsh (James Cook University, Australia) Lecture 1 – Introduction to Star Formation Throughout the Galaxy Lecture.

Suzaku Study of X-ray Emission from the Molecular Clouds in the Galactic Center M. Nobukawa, S. G. Ryu, S. Nakashima, T. G. Tsuru, K. Koyama (Kyoto Univ.),

Supermassive Black Holes at the Centers of Galaxies Singles and Pairs using X-rays to study black holes disruption of stars by massive black holes pairs.

Do flares in Sagittarius A* reflect the last stage of tidal capture? Andrej Čadež 1, Massimo Calvani 2, Andreja Gomboc 1, Uroš Kostić 1 1 University of.

Copyright © 2012 Pearson Education, Inc. Chapter 14 Our Galaxy.

Renaissance: Formation of the first light sources in the Universe after the Dark Ages Justin Vandenbroucke, UC Berkeley Physics 290H, February 12, 2008.

October 20, 2005 Nearly Resolved Debris Disks STScI, Baltimore Hervé Beust Laboratoire d’Astrophysique de Grenoble, France FOST group The origin of the.

15.4 Quasars and Other Active Galactic Nuclei Our Goals for Learning What are quasars? What is the power source for quasars and other active galactic nuclei?

Gamma-Ray Bursts Energy problem and beaming * Mergers versus collapsars GRB host galaxies and locations within galaxy Supernova connection Fireball model.

ASTR112 The Galaxy Lecture 7 Prof. John Hearnshaw 11. The galactic nucleus and central bulge 11.1 Infrared observations (cont.) 11.2 Radio observations.

Photoevaporative Mass Loss From Hot Jupiters Ruth Murray-Clay Eugene Chiang UC Berkeley.

Chapter 19 Our Galaxy.

Galaxies with Active Nuclei Chapter 14:. Active Galaxies Galaxies with extremely violent energy release in their nuclei (pl. of nucleus).  “active galactic.

Active Galactic Nuclei Chapter 25 Revised Active Galactic Nuclei Come in several varieties; Starburst Nuclei – Nearby normal galaxies with unusually.

HBT 28-Jun-2005 Henry Throop Department of Space Studies Southwest Research Institute (SwRI) Boulder, Colorado John Bally University of Colorado Portugal,

The AU Mic Debris Ring Density profiles & Dust Dynamics J.-C. Augereau & H. Beust Grenoble Observatory (LAOG)

The Milky Way Galaxy. Sky Maps in Different Bands.

AST101 Lecture 19 Discovery of the Galaxy. Northern Milky Way.

The Character of High Energy Emission From The Galactic Binary LS Andy Smith Smithsonian Astrophysical Observatory (for the VERITAS collaboration)

Copyright © 2010 Pearson Education, Inc. Chapter 14 The Milky Way Galaxy Lecture Outline.

Super Massive Black Holes The Unknown Astrophysics of their initial formation.

QUIET BHs in GALACTIC NUCLEI Random motions of stars –measure random speeds, look for cusps –example: Milky Way nucleus, M87 Organized rotation of stars.

The Birth of Stars and Planets in the Orion Nebula K. Smith (STScI)

SgrA* and the central cluster in NIR S. Trippe, T. Ott, F. Eisenhauer, T. Paumard, F. Martins, S. Gillessen, R. Genzel, R. Schödel, A. Eckart, T. Alexander,

“Globular” Clusters: M15: A globular cluster containing about 1 million (old) stars. distance = 10,000 pc radius  25 pc “turn-off age”  12 billion years.

Tidal Disruption Events

Lecture 30- The Structure of the Milky Way Galaxy

A cloud of gas falling towards the central black hole in the Milky Way. Jordi Miralda Escudé ICREA, Institut de Ciències del Cosmos University of Barcelona.

An Overabundance of X-ray Binaries Near the Galactic Center

Young planetary systems

Peculiar (colliding) Galaxies and Active Galaxies

AGN: Quasars By: Jay Hooper.

Galaxies With Active Nuclei

Galaxies With Active Nuclei

Presentation transcript:

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* Ghez et al. 2008; Genzel et al (BH at rest in GC)

Gillessen et al., Nature (2012) *Ionized cloud, ~3x10^5 cm^{-3}, ~100AU, electrons at 10^4K, dust at 550K, 3 Earth masses

Latest Data Gillessen et al., submitted (2012)

Br-gamma slit SgrA*

Br-gamma

Burkert et al. (2012)

Schartmann et al. (2012) “Pressure-Confined Cloud” Model

Problem: why is the head moving on a ballistic orbit with no evidence for ambient ram-pressure?

Tidal Disruption of a Proto-Planetary Disk Around a Low-Mass Star Murray-Clay & Loeb (2012) *Planets form near SgrA* *Flags low-mass stars

Physical Parameters Low-mass star, born in circum-nuclear ring at ~0.04pc, and scattered into orbit a few Myrs ago. Original Current

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:

ionized observednow Br- pericenter HI observed

Hypervelocity Planets from Tidal Disruption of Stellar Binaries by SgrA* Ginsburg, Loeb, & Wegner (2012)

Possible Outcome: Free Hypervelocity Planets

2 planets 0.02 AU 4 planets 0.02 AU 0.03AU Probabilities of Outcomes

Transits of Hypervelocity Stars

Tidal Flares from Disrupted Planets or Asteroids Waste dump: source of clean energy for galacto-centeric civilizations

Tidal Distruption of a Bound Object (e=0.8,beta=5) Hayasaki, Stone, and Loeb 2012

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.

Initial Ring Results in Two Bright Spots

A Relativistic Jet from a TDE: Swift (GRB110328A) *Synchrotron and X-ray peaks are emitted from different regions; bulk Lorentz factor~2-3 Bloom et al. 2011Zauderer et al. 2011