Kepler’s Third Law and the Masses of Black Holes

2020 ◽  
Author(s):  
Alan Hirshfeld
Keyword(s):  
Black Holes ◽  
Third Law ◽  
The Masses

scholarly journals Toward Precision Measurement of Central Black Hole Masses

2009 ◽  
Vol 5 (S267) ◽  
pp. 151-160 ◽  
Author(s):  
Bradley M. Peterson
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Host Galaxy ◽  
Reverberation Mapping ◽  
Line Region ◽  
The Masses ◽  
The Relationship ◽  
Black Hole Masses ◽  
Intrinsic Scatter ◽  
Direct And Indirect Methods

AbstractWe review briefly direct and indirect methods of measuring the masses of black holes in galactic nuclei, and then focus attention on supermassive black holes in active nuclei, with special attention to results from reverberation mapping and their limitations. We find that the intrinsic scatter in the relationship between the AGN luminosity and the broad-line region size is very small, ~0.11 dex, comparable to the uncertainties in the better reverberation measurements. We also find that the relationship between reverberation-based black hole masses and host-galaxy bulge luminosities also seems to have surprisingly little intrinsic scatter, ~0.17 dex. We note, however, that there are still potential systematics that could affect the overall mass calibration at the level of a factor of a few.

scholarly journals The central dynamics of M3, M13, and M92: stringent limits on the masses of intermediate-mass black holes

2014 ◽  
Vol 566 ◽  
pp. A58 ◽  
Author(s):  
S. Kamann ◽  
L. Wisotzki ◽  
M. M. Roth ◽  
J. Gerssen ◽  
T.-O. Husser ◽  
...  
Keyword(s):  
Black Holes ◽  
Intermediate Mass ◽  
The Masses ◽  
Intermediate Mass Black Holes

The Biggest Ears in the Sky: LIGO

2020 ◽  
pp. 108-136
Author(s):  
John W. Moffat
Keyword(s):  
Black Holes ◽  
Gravitational Waves ◽  
Nobel Prize ◽  
Executive Director ◽  
Numerical Relativity ◽  
Washington State ◽  
Wave Form ◽  
Press Conference ◽  
The Masses ◽  
First Time

At a press conference on February 11, 2016, David Reitz, LIGO Executive Director, announced, “We did it!” They detected gravitational waves for the first time. Both LIGO sites, in Washington state and Louisiana, registered the incoming gravitational waves from two black holes colliding and merging far away. Over the following months, more mergers were detected. Gravitational waves are caused by the acceleration of a massive object, which stretches and compresses spacetime in a wave-like motion that is incredibly small and difficult to detect. Numerical relativity research over decades has produced over a quarter of a million template solutions of Einstein’s equations. The best template fit to the wave form data identifies the masses and spins of the two merging black holes. Much of this chapter describes the technology of the LIGO apparatus. On October 3, 2017, Barish, Thorne, and Weiss, the founders of LIGO, received the Nobel Prize for Physics.

scholarly journals Orbital Motions in Binary Protostellar Systems

2004 ◽  
Vol 191 ◽  
pp. 92-99
Author(s):  
L.F. Rodríguez
Keyword(s):  
Nuclear Reactions ◽  
Molecular Complexes ◽  
Close Approach ◽  
Young Star ◽  
Double Star ◽  
Large Array ◽  
Very Large Array ◽  
Low Mass ◽  
Third Law ◽  
The Masses

AbstractUsing high-resolution (~ 01), multi-epoch Very Large Array observations, we have detected orbital motions in several low-luminosity protobinary systems in the Taurus and ρ Ophiuchus molecular complexes. The masses obtained from Kepler’s third law are of the order of 0.5 to 2 M⊙, as expected for such low-mass protostars. The relatively large bolometric luminosities of these young systems corroborates the notion that protostars obtain most of their luminosity from accretion and not from nuclear reactions. In addition, in one of the sources studied (a multiple system in Taurus), a low-mass young star has shown a drastic change in its orbit after a close approach with another component of the system, presumed to be a double star. The large proper motion achieved by this low mass protostar (20 km s−1), suggests an ejection from the system.

scholarly journals Black hole high mass X-ray binary microquasars at cosmic dawn

2018 ◽  
Vol 14 (S346) ◽  
pp. 365-379 ◽  
Author(s):  
I. F. Mirabel
Keyword(s):  
Black Holes ◽  
Theoretical Models ◽  
High Mass ◽  
Cosmic Radio ◽  
X Rays ◽  
Binary Black Holes ◽  
Relativistic Jet ◽  
Large Populations ◽  
Radio Background ◽  
The Masses

AbstractTheoretical models and observations suggest that primordial Stellar Black Holes (Pop-III-BHs) were prolifically formed in HMXBs, which are powerful relativistic jet sources of synchrotron radiation called Microquasars (MQs).Large populations of BH-HMXB-MQs at cosmic dawn produce a smooth synchrotron cosmic radio background (CRB) that could account for the excess amplitude of atomic hydrogen absorption at z∼17, recently reported by EDGES.BH-HMXB-MQs at cosmic dawn precede supernovae, neutron stars and dust. BH-HMXB-MQs promptly inject into the IGM hard X-rays and relativistic jets, which overtake the slowly expanding HII regions ionized by progenitor Pop-III stars, heating and partially ionizing the IGM over larger distance scales.BH-HMXBs are channels for the formation of Binary-Black-Holes (BBHs). The large masses of BBHs detected by gravitational waves, relative to the masses of BHs detected by X-rays, and the high rates of BBH-mergers, are consistent with high formation rates of BH-HMXBs and BBHs in the early universe.

scholarly journals UPPER LIMITS ON THE MASSES OF 105 SUPERMASSIVE BLACK HOLES FROMHUBBLE SPACE TELESCOPE/SPACE TELESCOPE IMAGING SPECTROGRAPH ARCHIVAL DATA

2009 ◽  
Vol 692 (1) ◽  
pp. 856-868 ◽  
Author(s):  
A. Beifiori ◽  
M. Sarzi ◽  
E. M. Corsini ◽  
E. Dalla Bontà ◽  
A. Pizzella ◽  
...  
Keyword(s):  
Black Holes ◽  
Supermassive Black Holes ◽  
Archival Data ◽  
Space Telescope ◽  
Upper Limits ◽  
The Masses ◽  
Imaging Spectrograph

scholarly journals On the masses of OJ287 black holes

2012 ◽  
Vol 427 (1) ◽  
pp. 77-83 ◽  
Author(s):  
M. J. Valtonen ◽  
S. Ciprini ◽  
H. J. Lehto
Keyword(s):  
Black Holes ◽  
The Masses

scholarly journals Distinction between distribution of masses of Wolf-Rayet stars and that of relativistic objects

2003 ◽  
Vol 212 ◽  
pp. 372-376
Author(s):  
Anatol M. Cherepashchuk
Keyword(s):  
Magnetic Field ◽  
Black Holes ◽  
Mass Loss ◽  
Loss Rate ◽  
Mass Loss Rate ◽  
Continuous Distribution ◽  
Core Mass ◽  
The Masses ◽  
Dependent Mass ◽  
Mass Dependent

The final masses MCO,f for the CO-cores of WR stars with known masses are calculated taking into account mass-dependent mass loss of WR stars and clumping structure of the WR wind which allows the mass loss rate to be decreased by a factor of 3. The masses of MCO,f lie in the range (1-2) - (20-44)M⊙ and have continuous distribution in contrast with distribution of masses Mx of relativistic objects. The distribution of Mx seems to be bimodal with a gap in the range Mx = 2-4 M⊙. A mean CO-core mass <MCO,f = 7.4-10.3 M⊙ is close to that of black holes: <MBH = 8-10 M⊙. Difference between distributions of MCO,f and Mx allows us to suggest that the nature of a formed relativistic object (neutron star, black hole) is determined not only by the mass of a progenitor but also by some other parameters: rotation, magnetic field, etc.

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