31 research outputs found
The Gravothermal Instability at all scales: from Turnaround Radius to Supernovae
The gravitational instability, responsible for the formation of the structure
of the Universe, occurs below energy thresholds and above spatial scales of a
self-gravitating expanding region, when thermal energy can no longer
counterbalance self-gravity. I argue that at sufficiently-large scales, dark
energy may restore thermal stability. This stability re-entrance of an
isothermal sphere defines a turnaround radius, which dictates the maximum
allowed size of any structure generated by gravitational instability. On the
opposite limit of high energies and small scales, I will show that an ideal,
quantum or classical, self-gravitating gas is subject to a high-energy
relativistic gravothermal instability. It occurs at sufficiently-high energy
and small radii, when thermal energy cannot support its own gravitational
attraction. Applications of the phenomenon include neutron stars and
core-collapse supernovae. I also extend the original Oppenheimer--Volkov
calculation of the maximum mass limit of ideal neutron cores to the non-zero
temperature regime, relevant to the whole cooling stage from a hot
proto-neutron star down to the final cold state.Comment: Minor amendments to match published versio
Binary black hole growth by gas accretion in stellar clusters
We show that binaries of stellar-mass black holes formed inside a young
protoglobular cluster, can grow rapidly inside the cluster's core by accretion
of the intracluster gas, before the gas may be depleted from the core. A black
hole with mass of the order of eight solar masses can grow to values of the
order of thirty five solar masses in accordance with recent gravitational waves
signals observed by LIGO. Due to the black hole mass increase, a binary may
also harden. The growth of binary black holes in a dense protoglobular cluster
through mass accretion indicates a potentially important formation and
hardening channel
Relativistic Gravothermal Instabilities
The thermodynamic instabilities of the self-gravitating, classical ideal gas
are studied in the case of static, spherically symmetric configurations in
General Relativity taking into account the Tolman-Ehrenfest effect. One type of
instabilities is found at low energies, where thermal energy becomes too weak
to halt gravity and another at high energies, where gravitational attraction of
thermal pressure overcomes its stabilizing effect. These turning points of
stability are found to depend on the total rest mass over the
radius . The low energy instability is the relativistic generalization of
Antonov instability, which is recovered in the limit
and low temperatures, while in the same limit and high temperatures, the high
energy instability recovers the instability of the radiation equation of state.
In the temperature versus energy diagram of series of equilibria, the two types
of gravothermal instabilities make themselves evident as a double spiral! The
two energy limits correspond also to radius limits. So that, stable static
configurations exist only in between two marginal radii for any fixed energy
with negative thermal plus gravitational energy. Ultimate limits of rest mass,
as well as total mass-energy, are reported. Applications to neutron cores are
discussed.Comment: 30 pages, 21 figures; references added; minor changes to match
published versio
Binary Black Hole Growth by Gas Accretion in Stellar Clusters
We show that binaries of stellar-mass black holes formed inside a young protoglobular cluster, can grow rapidly inside the clusters core by accretion of the intracluster gas, before the gas may be depleted from the core. A black hole with mass of the order of eight solar masses can grow to values of the order of thirty five solar masses in accordance with recent gravitational waves signals observed by LIGO. Due to the black hole mass increase, a binary may also harden. The growth of binary black holes in a dense protoglobular cluster through mass accretion indicates a potentially important formation and hardening channel
The Cosmological Black Hole
We briefly review the recent novel solution of General Relativity, we call
the cosmological black hole, firstly discovered in [Roupas, Z. Eur. Phys. J. C
82, 255 (2022)]. A dark energy universe and a Schwartzschild black hole are
matched on a common dual event horizon which is finitely thick due to quantum
indeterminacy. The system gets stabilized by a finite tangential pressure
applied on the dual horizon. The fluid entropy of the system at a Tolman
temperature identified with the cosmological horizon temperature is calculated
to be equal with the Bekenstein-Hawking entropy.Comment: Talk given in the 11th International Conference on Mathematical
Modelling in Physical Science