Celiac disease and adverse reactions to food

Lippai, G; Dékány, K; Szentkereszty, B; Mármarosi, I; Schandl, László

doi:10.1055/s-2004-826985

Cited by 10 publications

(17 citation statements)

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“…As shown numerically for the first time by Lippai et al (2008), and then confirmed repeatedly by several authors (O'Neill et al, 2009;Corrales et al, 2010;Rossi et al, 2010;Megevand et al, 2009;Anderson et al, 2010;Zanotti et al, 2010), the combined effects of mass loss from the central black hole and of the recoil velocity generate a spiral shock pattern that transports angular momentum outwards, and become responsible of an enhanced luminosity 3 . Figure 1 shows the iso-density curves of the rest mass density in the two models CoRot a.0.9 and CounterRot a.0.9, plotted when the emitted luminosity reaches its maximum.…”

Section: Resultsmentioning

confidence: 67%

“…During the post-merger phase, it is not clear whether a retrograde disc may have significant effects on both the dynamics and the EM signal emitted by the system. Several time dependent numerical investigations of prograde circumbinary discs in the post-merger phase have been performed, both in a Newtonian (Lippai et al, 2008;O'Neill et al, 2009;Corrales et al, 2010;Rossi et al, 2010) and in a relativistic framework (Megevand et al, 2009;Anderson et al, 2010;Zanotti et al, 2010). With different emphasis and caveats, the majority of these works have confirmed the possibility of detecting a significant EM counterpart from SMBBHs.…”

Section: Introductionmentioning

confidence: 99%

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Electromagnetic counterparts from counter-rotating relativistic kicked discs

Zanotti

2012

New Astronomy

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We show the results of two dimensional general relativistic inviscid and isothermal hydrodynamical simulations comparing the behavior of co-rotating (with respect to the black hole rotation) and counter-rotating circumbinary quasi-Keplerian discs in the post merger phase of a supermassive binary black hole system. While confirming the spiral shock generation within the disc due to the combined effects of mass loss and recoil velocity of the black hole, we find that the maximum luminosity of counter-rotating discs is a factor ∼ (2 − 12) higher than in the co-rotating case, depending on the spin of the black hole. On the other hand, the luminosity peak happens ∼ 10 days later with respect to the co-rotating case. Although the global dynamics of counter-rotating discs in the post merger phase of a merging event is very similar to that for co-rotating discs, an important difference has been found. In fact, increasing the spin of the central black hole produces more luminous co-rotating discs while less luminous counter-rotating ones.

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Section: Resultsmentioning

confidence: 67%

Section: Introductionmentioning

confidence: 99%

Electromagnetic counterparts from counter-rotating relativistic kicked discs

Zanotti

2012

New Astronomy

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“…The electromagnetic signature of a recoiling BH, detailed in this paper, is different from the one expected in the immediate vicinity of a coalescence event. Electromagnetic afterglows of LISA coalescence events (Milosavljević & Phinney 2005;Kocsis & Loeb 2008;Lippai, Frei & Haiman 2008) have peculiar off-on time-dependent features varying on much shorter times and spatial scales.…”

Section: S U M M a Ry A N D Discussionmentioning

confidence: 99%

Imprints of recoiling massive black holes on the hot gas of early-type galaxies

Devecchi¹,

Rasia²,

Dotti³

et al. 2009

Monthly Notices of the Royal Astronomical Society

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Anisotropic gravitational radiation from a coalescing black hole (BH) binary is known to impart recoil velocities of up to ∼1000 km s−1 to the remnant BH. In this context, we study the motion of a recoiling BH inside a galaxy modelled as a Hernquist sphere, and the signature that the hole imprints on the hot gas, using N‐body/smoothed particle hydrodynamics simulations. Ejection of the BH results in a sudden expansion of the gas ending with the formation of a gaseous core, similarly to what is seen for the stars. A cometary tail of particles bound to the BH is initially released along its trail. As the BH moves on a return orbit, a nearly spherical swarm of hot gaseous particles forms at every apocentre: this feature can live up to ≈108 years. If the recoil velocity exceeds the sound speed initially, the BH shocks the gas in the form of a Mach cone in density near each supersonic pericentric passage. We find that the X‐ray fingerprint of a recoiling BH can be detected in Chandra X‐ray maps out to a distance of Virgo. For exceptionally massive BHs, the Mach cone and the wakes can be observed out to a few hundred of milliparsec. The detection of the Mach cone is of twofold importance as it can be a probe of high‐velocity recoils, and an assessment of the scatter of the MBH−Mbulge relation at large BH masses.

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“…A second source of perturbations in the disk comes from the loss of gravitational mass with the emission of gravitational radiation, weakening the gravitational potential felt by the disk. These effects, as discussed in [19,20,21], can induce possible emissions and some of these have been investigated in part in [20,21,22,23,24]. These works study the dy-namics of the disks when either mass reduction (due to the energy lost by the system) or recoil velocity (due to the asymmetric flux of gravitational radiation) effects are included and present preliminary estimates of emissions from the system with the goal of understanding possible observations in the electromagnetic spectrum.…”

Section: Introductionmentioning

confidence: 95%

Post-merger electromagnetic emissions from disks perturbed by binary black holes

et al. 2010

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We simulate the possible emission from a disk perturbed by a recoiling super-massive black hole.To this end, we study radiation transfer from the system incorporating bremsstrahlung emission from a Maxwellian plasma and absorption given by Kramer's opacity law modified to incorporate blackbody effects. We employ this model in the radiation transfer integration to compute the luminosity at several frequencies, and compare with previous bremsstrahlung luminosity estimations from a transparent limit (in which the emissivity is integrated over the computational domain and over all frequencies) and with a simple thermal emission model. We find close agreement between the radiation transfer results and the estimated bremsstrahlung luminosity from previous work for electromagnetic signals above 10 14 Hz. For lower frequencies, we find a self-eclipsing behavior in the disk, resulting in a strong intensity variability connected to the orbital period of the disk.

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Celiac disease and adverse reactions to food

Cited by 10 publications

References 0 publications

Electromagnetic counterparts from counter-rotating relativistic kicked discs

Electromagnetic counterparts from counter-rotating relativistic kicked discs

Imprints of recoiling massive black holes on the hot gas of early-type galaxies

Post-merger electromagnetic emissions from disks perturbed by binary black holes

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