Tidal squeezing of stars by Schwarzschild black holes

Luminet, Jean‐Pierre; Marck, J. A.

doi:10.1093/mnras/212.1.57

Cited by 106 publications

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“…For concreteness, we have assumed that the limiting radius is intermediate between the two extreme cases mentioned above; we have used the limit r T > 2r g . Yet another source of uncertainty derives from the fact that we have used Newtonian dynamics in our analysis, whereas it is clear that relativistic effects should be important (Luminet & Marck 1985;Laguna et al 1993;Frolov et al 1994;Diener et al 1997).…”

Section: Summary and Discussionmentioning

confidence: 99%

The Giant X‐Ray Flare of NGC 5905: Tidal Disruption of a Star, a Brown Dwarf, or a Planet?

Li¹,

Narayan²,

Menou³

2002

ApJ

124

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We model the 1990 giant X-ray flare of the quiescent galaxy NGC 5905 as the tidal disruption of a star by a supermassive black hole. From the observed rapid decline of the luminosity, over a timescale of a few years, we argue that the flare was powered by the fallback of debris rather than subsequent accretion via a thin disk. The fallback model allows constraints to be set on the black hole mass and the mass of debris. The latter must be very much less than a solar mass to explain the very low luminosity of the flare. The observations can be explained either as the partial stripping of the outer layers of a low-mass main-sequence star or as the disruption of a brown dwarf or a giant planet. We find that the X-ray emission in the flare must have originated within a small patch rather than over the entire torus of circularized material surrounding the black hole. We suggest that the patch corresponds to the '' bright spot '' where the stream of returning debris impacts the torus. Interestingly, although the peak luminosity of the flare was highly sub-Eddington, the peak flux from the bright spot was close to the Eddington limit. We speculate on the implications of this result for observations of other flare events.

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Section: Summary and Discussionmentioning

confidence: 99%

The Giant X‐Ray Flare of NGC 5905: Tidal Disruption of a Star, a Brown Dwarf, or a Planet?

Li¹,

Narayan²,

Menou³

2002

ApJ

124

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“…-If the stellar orbit is deeply plunging, the squeezing of the star can be extreme. If nuclear burning is ignited during this process, this would result in a GRB-like explosion (e.g., Luminet & Marck 1985, Carter & Luminet 1982). -Part of the disrupted star will be on unbound trajectories.…”

Section: Introductionmentioning

confidence: 99%

Tidal disruption of stars by supermassive black holes: The X-ray view

Komossa

2012

EPJ Web of Conferences

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Abstract. The tidal disruption of stars by supermassive black holes produces luminous soft X-ray accretion flares in otherwise inactive galaxies. First events have been discovered in X-rays with the ROSAT observatory, and have more recently been detected with XMM-Newton, Chandra and Swift, and at other wavelengths. In X-rays, they typically appear as very soft, exceptionally luminous outbursts of radiation, which decline consistent with L ∝ t −5/3 on the timescale of months to years. They reach total amplitudes of decline up to factors 1000-6000 more than a decade after their initial high-states, and in low-state, their host galaxies are essentially X-ray inactive, optically inactive, and radio inactive. X-ray luminous tidal disruption events (TDEs) represent a powerful new probe of accretion physics near the event horizon, and of relativistic effects. TDEs offer a new way of estimating black hole spin, and they are signposts of supermassive binary black holes and recoiling black holes. Once discovered in the thousands in upcoming sky surveys, their rates will probe stellar dynamics in distant galaxies, and they will uncover theso far elusive -population of intermediate mass black holes in the universe, if they do exist. Further, the reprocessing of the flare into IR, optical and UV emission lines provides us with multiple new diagnostics of the properties of any gaseous material in the vicinity of the black hole (including the disrupted star itself) and in the host galaxy. First candidate events of this kind have been reported recently.

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“…Relativistic modifications on the stellar orbit and on the tidal field significantly appear when the star approaches the black hole's gravitational radius. Due to relativistic precession, the parabolic-type orbit must eventually intersect once in the Schwarzschild space-time, and depending on the position of the crossing point, the star can be subjected to several successive compressions during its motion within the tidal radius (Luminet & Marck 1985;Laguna et al 1993).…”

Section: Resultsmentioning

confidence: 99%

Relativistic tidal compressions of a star by a massive black hole

Brassart

Luminet

2010

A&A

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Aims. We investigate the stellar pancake mechanism during which a solar-type star is tidally flattened within its orbital plane as it passes close to a 10 6 M black hole. Methods. We simulated the relativistic orthogonal compression process and follow the associated shock waves formation. We considered a one-dimensional hydrodynamical stellar model moving in the relativistic gravitational field of a non-rotating black hole. The model is numerically solved using a Godunov-type shock-capturing source-splitting method to correctly reproduce the shock wave profiles. Results. Simulations confirm that the space-time curvature can induce several successive orthogonal compressions of the star, which give rise to several strong shock waves. The shock waves finally escape from the star and repeatedly heat up the stellar surface to high-energy values. Such a shock-heating could interestingly provide a direct observational signature of strongly disruptive starblack hole encounters through the emission of hard X or soft γ-ray bursts. Timescales and energies of such a process are consistent with some observed events such as GRB 970815.

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Tidal squeezing of stars by Schwarzschild black holes

Cited by 106 publications

References 0 publications

The Giant X‐Ray Flare of NGC 5905: Tidal Disruption of a Star, a Brown Dwarf, or a Planet?

The Giant X‐Ray Flare of NGC 5905: Tidal Disruption of a Star, a Brown Dwarf, or a Planet?

Tidal disruption of stars by supermassive black holes: The X-ray view

Relativistic tidal compressions of a star by a massive black hole

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