Dynamics of the Star S0‐1 and the Nature of the Compact Dark Object at the Galactic Center

Munyaneza, Faustin; Tsiklauri, David; Viollier, Raoul D.

doi:10.1086/308026

Cited by 23 publications

(12 citation statements)

References 44 publications

(67 reference statements)

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“…While some of these arguments offer supportive, rather than direct, evidence for the existence of the black hole, future determinations of the stellar orbits at the Galactic Center using space interferometry (e.g., with DARWIN; Wilson 2000) promise much more insight. These orbits may not help us to distinguish between rotating and non-rotating black holes, but they will clearly differentiate between point and extended mass distributions (Munyaneza, Tsiklauri, & Viollier 1999).…”

Section: Interactions Of Sgr A* With the Central Star Clustermentioning

confidence: 98%

The Supermassive Black Hole at the Galactic Center

Melia

Falcke

2001

Annu. Rev. Astron. Astrophys.

480

416

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The inner few parsecs at the Galactic Center have come under intense scrutiny in recent years, in part due to the exciting broad-band observations of this region, but also because of the growing interest from theorists motivated to study the physics of black hole accretion, magnetized gas dynamics and unusual star formation. The Galactic Center is now known to contain arguably the most compelling supermassive black hole candidate, weighing in at a little over 2.6 million suns. Its interaction with the nearby environment, comprised of clusters of evolved and young stars, a molecular dusty ring, ionized gas streamers, diffuse hot gas, and a hypernova remnant, is providing a wealth of accretion phenomenology and high-energy processes for detailed modeling. In this review, we summarize the latest observational results, and focus on the physical interpretation of the most intriguing object in this region---the compact radio source Sgr A*, thought to be the radiative manifestation of the supermassive black hole.Comment: Annual Review of Astronomy & Astrophysics, Vol. 39 (2001), in press, 48 pages, 20 figures (partially in reduced quality), also available at http://www.mpifr-bonn.mpg.de/staff/hfalcke/publications.html#gcrevie

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Section: Interactions Of Sgr A* With the Central Star Clustermentioning

confidence: 98%

The Supermassive Black Hole at the Galactic Center

Melia

Falcke

2001

Annu. Rev. Astron. Astrophys.

480

416

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“…The physics of degenerate FBs as a model of DM at the center of galaxies was considered in a series of papers (Bilić et al 2002a,b;Bilić et al 1999;Munyaneza et al 1998Munyaneza et al , 1999Munyaneza & Viollier 2002;; Viollier 1994). In these papers, it was argued that the supermassive compact objects in galactic centers are FBs rather than BHs.…”

Section: Black Hole Accretion Rate and Pauli Principlementioning

confidence: 99%

Fast growth of supermassive black holes in galaxies

Munyaneza¹,

Biermann²

2005

A&A

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Abstract. We report on a calculation of the growth of the mass of supermassive black holes at galactic centers from dark matter and Eddington -limited baryonic accretion. Assuming that dark matter halos are made of fermions and harbor compact degenerate Fermi balls of masses from 10 3 M to 10 6 M , we find that dark matter accretion can boost the mass of seed black holes from about ∼5 M to 10 3−4 M black holes, which then grow by Eddington-limited baryonic accretion to supermassive black holes of 10 6−9 M . We then show that the formation of the recently detected supermassive black hole of 3 × 10 9 M at a redshift of z = 6.41 in the quasar SDSS J114816.64+525150.3 could be understood if the black hole completely consumes the degenerate Fermi ball and then grows by Eddington-limited baryonic accretion. In the context of this model we constrain the dark matter particle masses to be within the range from 12 keV/c 2 to about 450 keV/c 2 . Finally we investigate the black hole growth dependence on the formation time and on the mass of the seed black hole. We find that in order to fit the observed data point of M BH ∼ 3 × 10 9 M and z ∼ 6.41, dark matter accretion cannot start later than about 2 × 10 8 years and the seed BH cannot be greater than about 10 4 M . Our results are in full agreement with the WMAP observations that indicate that the first onset of star formation might have occurred at a redshift of z ∼ 15−20. For other models of dark matter particle masses, corresponding constraints may be derived from the growth of black holes in the center of galaxies.

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“…(iii) The FB scenario provides a natural cut-off of the emitted radiation at infrared frequencies ∼ > 10 13 GHz, as is actually observed in the spectrum of the Galactic center (Bilić, Tsiklauri and Viollier 1998;Tsiklauri and Viollier 1999;Munyaneza and Viollier 1999). This is because matter, e.g.…”

Section: The Case For Degenerate Fermion Ballsmentioning

confidence: 79%

The Motion of Stars near the Galactic Center: A Comparison of the Black Hole and Fermion Ball Scenarios

Munyaneza

Viollier

2002

ApJ

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After a discussion of the properties of degenerate fermion balls, we analyze the orbits of the stars S0-1 and S0-2, which have the smallest projected distances to Sgr A * , in the supermassive black hole as well as in the fermion ball scenarios of the Galactic center. It is shown that both scenarios are consistent with the data, as measured during the last six years by Genzel et al. and Ghez et al. The free parameters of the projected orbit of a star are the unknown components of its velocity v z and distance z to Sgr A * in 1995.4, with the z-axis being in the line of sight. We show, in the case of S0-1 and S0-2, that the z − v z phasespace, which fits the data, is much larger for the fermion ball than for the black hole scenario. Future measurements of the positions or radial velocities of S0-1 and S0-2 could reduce this allowed phase-space and eventually rule out one of the currently acceptable scenarios. This may shed some light into the nature of the supermassive compact dark object, or dark matter in general at the center of our Galaxy.

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Dynamics of the Star S0‐1 and the Nature of the Compact Dark Object at the Galactic Center

Cited by 23 publications

References 44 publications

The Supermassive Black Hole at the Galactic Center

The Supermassive Black Hole at the Galactic Center

Fast growth of supermassive black holes in galaxies

The Motion of Stars near the Galactic Center: A Comparison of the Black Hole and Fermion Ball Scenarios

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