848 research outputs found
A star disrupted by a stellar black hole as the origin of the cloud falling toward the Galactic center
We propose that the cloud moving on a highly eccentric orbit near the central
black hole in our Galaxy, reported by Gillessen et al., is formed by a
photoevaporation wind originating in a disk around a star that is tidally
perturbed and shocked at every peribothron passage. The disk is proposed to
have formed when a stellar black hole flew by the star, tidally disrupted its
envelope, and placed the star on its present orbit with some of the tidal
debris forming a disk. A disrupting encounter at the location of the observed
cloud is most likely to be caused by a stellar black hole because of the
expected dynamical mass segregation; the rate of these disk-forming encounters
may be as high as per year. The star should also be spun up by
the encounter, so the disk may subsequently expand by absorbing angular
momentum from the star. Once the disk expands up to the tidal truncation
radius, the tidal perturbation of the outer disk edge at every peribothron may
place gas streams on larger orbits which can give rise to a photoevaporation
wind that forms the cloud at every orbit. This model predicts that, after the
cloud is disrupted at the next peribothron passage in 2013, a smaller
unresolved cloud will gradually grow around the star on the same present orbit.
An increased infrared luminosity from the disk may also be detectable when the
peribothron is reached. We also note that this model revives the encounter
theory for planet formation.Comment: To be published in Ap
`First Light' in the Universe; What Ended the "Dark Age"?
The universe would have been completely dark between the epoch of
recombination and the development of the first non-linear structure. But at
redshifts beyond 5 -- perhaps even beyond 20 -- stars formed within
`subgalaxies' and created the first heavy elements; these same systems
(together perhaps with `miniquasars') generated the UV radiation that ionized
the IGM, and maybe also the first significant magnetic fields. Although we can
already probe back to , these very first objects may be so faint
that their detection must await next-generation optical and infrared
telescopes. Observations in other wavebands may offer indirect clues to when
reionization occurred. Despite the rapid improvements in numerical simulations,
the processes of star formation and feedback are likely to remain a challenge
for the next decade.Comment: For ``Physics Reports'' special issue in memory of D.N. Schram
Microlensing of Extremely Magnified Stars near Caustics of Galaxy Clusters
Recent observations of lensed galaxies at cosmological distances have
detected individual stars that are extremely magnified when crossing the
caustics of lensing clusters. In idealized cluster lenses with smooth mass
distributions, two images of a star of radius approaching a caustic
brighten as and reach a peak magnification before merging on the critical curve. We show that a mass
fraction () in microlenses inevitably
disrupts the smooth caustic into a network of corrugated microcaustics, and
produces light curves with numerous peaks. Using analytical calculations and
numerical simulations, we derive the characteristic width of the network,
caustic-crossing frequencies, and peak magnifications. For the lens parameters
of a recent detection and a population of intracluster stars with , we find a source-plane width of for the
caustic network, which spans on the image plane. A source
star takes years to cross this width, with a total of crossings, each one lasting for with typical peak magnifications of . The exquisite sensitivity of caustic-crossing
events to the granularity of the lens-mass distribution makes them ideal probes
of dark matter components, such as compact halo objects and ultralight axion
dark matter.Comment: 29 pages, 11 figures, 2 tables; changed to match published versio
Soft X-ray Absorption by High-Redshift Intergalactic Helium
The Lyman alpha absorption from intergalactic, once-ionized helium (HeII) has
been measured with HST in four quasars over the last few years, over the
redshift range 2.4 < z < 3.2. These observations have indicated that the HeII
reionization may not have been completed until z\simeq 2.8, and that large
fluctuations in the intensity of the HeII-ionizing background were present
before this epoch. The detailed history of HeII reionization at higher
redshifts is, however, model-dependent and difficult to determine from these
observations, because the IGM can be completely optically thick to Lya photons
when only a small fraction of the helium remains as HeII. In addition, finding
quasars in which the HeII Lya absorption can be observed becomes increasingly
difficult at higher redshift, owing to the large abundance of hydrogen Lyman
limit systems.
It is pointed out here that HeII in the IGM should also cause detectable
continuum absorption in the soft X-rays. The spectrum of a high-redshift source
seen behind the IGM when most of the helium was HeII should recover from the
HeII Lyman continuum absorption at an observed energy \sim 0.1 keV. Galactic
absorption will generally be stronger, but not by a large factor; the
intergalactic HeII absorption can be detected as an excess over the expected
Galactic absorption from the 21cm HI column density. In principle, this method
allows a direct determination of the fraction of helium that was singly ionized
as a function of redshift, if the measurement is done on a large sample of
high-redshift sources over a range of redshift.Comment: accepted to The Astrophysical Journal Letter
The star capture model for fueling quasar accretion disks
Although the powering mechanism for quasars is now widely recognized to be
the accretion of matter in a geometrically thin disk, the transport of matter
to the inner region of the disk where luminosity is emitted remains an unsolved
question. Miralda-Escud\'e & Kollmeier (2005) proposed a model whereby quasars
are fuelled when stars are captured by the accretion disk as they plunge
through the gas. Such plunging stars can then be destroyed and deliver their
mass to the accretion disk.
Here we present the first detailed calculations for the capture of stars
originating far from the accretion disk near the zone of influence of the
central black hole. In particular we examine the effect of adding a perturbing
mass to a fixed stellar cusp potential on bringing stars into the accretion
disk where they can be captured. The work presented here will be discussed in
detail in an upcoming publication Kennedy et al. (2010).Comment: 2 pages, 1 figure, to be published in Proceedings of IAU Symp. 271,
Astrophysical Dynamics: from Stars to Galaxies, ed. N. Brummell & A.S.
Brun, Cambrige Univ Pres
The Distribution of Mass and Gas in the Center of Clusters of Galaxies Implied by X-Ray and Lensing Observations
Observations of gravitational lensing indicate that the mass distribution in
clusters of galaxies (where most of the mass is dark matter) is highly peaked
towards the center, while X-ray observations imply that the gas is more
extended. The additional fact that the gas is cooling in the center has often
led one to expect that the gas temperature should be lower near the center, and
therefore the gas should be more concentrated than the dark matter. We show
that such expectation is not correct, and that the gas temperature must remain
approximately constant within the cooling region in order to have consistency
with the observed X-ray profiles and lenses. A multiphase cooling flow
naturally produces an approximately constant temperature profile, and a more
extended distribution for the gas compared to the mass. Cool phases are
deposited at relatively large radius, while hot phases are adiabatically heated
as they flow inwards and can keep the average temperature constant. Thus,
cooling flows result in an {\it increase} of the central temperature, relative
to a case where there is no cooling and the gas follows the mass distribution.
The increased central temperatures caused by cooling flows give a
characteristic core radius to the gas profiles, which is of order the cooling
radius. This provides a natural explanation for the typical cores observed in
X-ray clusters. It also brings into better agreement with observations the rate
of cluster evolution expected in self-similar hierarchical models. We propose
that clusters having core radii much larger than their cooling radii are in the
process of merging and are not in dynamical equilibrium.Comment: 30 pages, PostScrip
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