13 research outputs found
Astrophysical Axion Bounds
Axion emission by hot and dense plasmas is a new energy-loss channel for
stars. Observational consequences include a modification of the solar
sound-speed profile, an increase of the solar neutrino flux, a reduction of the
helium-burning lifetime of globular-cluster stars, accelerated white-dwarf
cooling, and a reduction of the supernova SN 1987A neutrino burst duration. We
review and update these arguments and summarize the resulting axion
constraints.Comment: Contribution to Axion volume of Lecture Notes in Physics, 20 pages, 3
figure
Comparing the asteroseismic properties of pulsating extremely low-mass pre-white dwarf stars and
We present the first results of a detailed comparison between the pulsation properties of pulsating Extremely Low-Mass pre-white dwarf stars (the pre-ELMV variable stars) and δ Scuti stars. The instability domains of these very different kinds of stars nearly overlap in the log Teff vs. log g diagram, leading to a degeneracy in the classification of the stars. Our aim is to provide asteroseismic tools for their correct classification
First axion bounds from a pulsating helium-rich white dwarf star
The Peccei-Quinn mechanism proposed to solve the CP problem of Quantum
Chromodynamics has as consequence the existence of axions, hypothetical weakly
interacting particles whose mass is constrained to be on the sub-eV range. If
these particles exist and interact with electrons, they would be emitted from
the dense interior of white dwarfs, becoming an important energy sink for the
star. Due to their well known physics, white dwarfs are good laboratories to
study the properties of fundamental particles such as the axions. We study the
general effect of axion emission on the evolution of helium-rich white dwarfs
and on their pulsational properties. To this aim, we calculate evolutionary
helium-rich white dwarf models with axion emission, and asses the pulsational
properties of this models. Our results indicate that the rates of change of
pulsation periods are significantly affected by the existence of axions. We are
able for the first time to independently constrain the mass of the axion from
the study of pulsating helium-rich white dwarfs. To do this, we use an
estimation of the rate of change of period of the pulsating white dwarf PG
1351+489 corresponding to the dominant pulsation period. From an
asteroseismological model of PG 1351+489 we obtain
for the axion-electron coupling constant, or 11.5
meV for the axion mass. This constraint is relaxed to
( 19.5 meV), when no
detailed asteroseismological model is adopted for the comparison with
observations.Comment: 17 pages, 6 figures, 2 tables, prepared for submission to JCA
Asteroseismology of pulsating DA white dwarfs with fully evolutionary models
We present a new approach for asteroseismology of DA white dwarfs that consists in the employment of a large set of non-static, physically sound, fully evolutionary models representative of these stars. We already have applied this approach with success to pulsating PG1159 stars (GW Vir variables). Our white dwarf models, which cover a wide range of stellar masses, effective temperatures, and envelope thicknesses, are the result of fully evolutionary computations that take into account the complete history of the progenitor stars from the ZAMS. In particular, the models are characterized by self-consistent chemical structures from the centre to the surface, a crucial aspect of white dwarf asteroseismology. We apply this approach to an ensemble of 44 bright DAV (ZZ Ceti) stars
Discovery, TESS Characterization, and Modeling of Pulsations in the Extremely Low-mass White Dwarf GD 278
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Contains fulltext :
240947.pdf (Author’s version preprint ) (Open Access
A consistency test of white dwarf and main sequence ages: NGC 6791
NGC 6791 is an open cluster that it is so close to us that can be imaged down to very faint luminosities. The main sequence turn-off age (∼8 Gyr) and the age derived from the cut-off of the white dwarf luminosity function (∼6 Gyr) were found to be significantly different. Here we demonstrate that the origin of this age discrepancy lies in an incorrect evaluation of the white dwarf cooling ages, and we show that when the relevant physical separation processes are included in the calculation of white dwarf sequences both ages are coincident