The rate of period change in DAV stars

Chen, Y. H.; Chen, Ding; Na, W. W.; Hong, Shu

doi:10.1088/1674-4527/17/7/65

Cited by 2 publications

(1 citation statement)

References 72 publications

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“…G117-B15A, whose Ṗobs matches ṖSCM well within uncertainties [31] and its structure details have been determined by asteroseismology in Refs. [12,31,32]. Here we use the structure details from Table 5, Ref.…”

Section: Estimationsupporting

confidence: 59%

Probing the dark matter-electron interactions via hydrogen-atmosphere pulsating white dwarfs

Niu¹,

Li²,

Zong³

et al. 2018

Phys. Rev. D

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In Phys. Rev. D 98, 103023 (2018), a novel scenario was proposed to probe the interactions between dark matter (DM) particles and electrons, via hydrogen-atmosphere pulsating white dwarfs (DAVs) in globular clusters. The estimation showed that the scenario could hopefully test the parameter space: 5 GeV < ∼ mχ < ∼ 10 4 GeV and σχ,e > ∼ 10 −40 cm 2 , where mχ is the DM particle's mass and σχ,e is the elastic scattering cross section between DM and electron. In this comment, we have determined the exact lower limit of the testable DM particle mass ∼ 1.38 − 1.58 GeV, which depends on σχ,e. This gives us a credible lower limit of the testable DM particle mass in above scenario, and provide a clear upper limit of the DM particle mass which we should consider in future research.In our previous work [1], we show that hydrogenatmosphere pulsating white dwarfs (DAVs) in globular clusters could be used as the probes to detect the interactions between dark matter (DM) and electrons. The potential sensitivity on DM particle's mass (m χ ) and elastic scattering cross section between DM and electron (σ χ,e ) could be hopefully extended to a region 5 GeV < ∼ m χ < ∼ 10 4 GeV and σ χ,e > ∼ 10 −40 cm 2 . The testable lowest mass (or the "evaporation mass" m evap ) there (5 GeV) was a conservative estimation based on the case that the evaporation effect could be ignored in the condition of Sun and DM-nucleon interactions [2,3]. Qualitatively speaking, m evap should be smaller in the case of DAV if we considered its stronger gravity potential, which makes it difficult for DM particles to evaporate. On the other hand, it should be larger if we considered the stronger interactions between electron than DM and nucleus, which makes it easier for DM particles to gain thermal kinetic energy from electrons. This should be calculated in details.Roughly speaking, we can estimate the evaporation mass by demanding that the typical velocity of a DM particle v χ = 2kT /m χ (where k is the Boltzmann constant and T is the typical temperature in the star) be equal to the local escape speed of the star v esc [4,5]. In this case, it gives the evaporation mass m evap ∼ 10 MeV, which is obviously smaller than the case in [1] 1 . But it is obvious that in this case, most parts of the DM particles in the star are disappeared by evaporation rather than annihilation. As a result, the real value of m evap , which represents the lower limit of m χ when the evaporation effect should be ignored, should be larger.Generally speaking, the evaporation mass should depend on the cross section between DM and the constituent of the star and the temperature distribution in it. Based on the work [6], following the detailed analytic expressions of the evaporation effect and the criterion to define m evap in it 2 , we determine the evaporation mass when 10 −41 cm 2 < ∼ σ χ,e < ∼ 10 −37 cm 2 and plot it in Fig. 1 (the black vertical dotted line).It shows that m evap ∼ 1.38−1.58 GeV, which is smaller than the estimation in [1] but much larger than the roughly estimation a...

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Section: Estimationsupporting

confidence: 59%

Probing the dark matter-electron interactions via hydrogen-atmosphere pulsating white dwarfs

Niu¹,

Li²,

Zong³

et al. 2018

Phys. Rev. D

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Asteroseismology of the DOV star PG 1159−035

Chen

2019

Monthly Notices of the Royal Astronomical Society

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Grids of DOV star models are evolved by WDEC with fixed atmospheric constituent to the spectral values of X C /X He /X O = 50/33/17. The core compositions are from white dwarf models at highest T ef f evolved by MESA. The eigenfrequencies are calculated and used to fit the observed modes. Based on 264.1 hours of photometric observations on PG 1159-035, Winget et al. identified 125 individual frequencies. Costa et al. identified 198 pulsation modes for PG 1159-035 according to the WET photometric data from 1983, 1985, 1989, and 2002. Both of them derived frequency splitting values of δσ l=1 ∼ 4.2 µHz and δσ l=2 ∼ 6.9 µHz. According to the values of δσ l=1 and δσ l=2 , 20 triplets and 9 quintuplets are selected and used to constrain the fitting models. Our optimal model has T ef f = 129000 K, M * = 0.63 M ⊙ , logg = 7.59, log(M env /M * ) = -5.0, and σ RMS = 1.97 s. The values of T ef f and logg are consistent with that values of Córsico et al.. The calculated modes of minimum rate of period change correspond to modes with maximum kinetic energy distributed in the envelope. The observed rates of period change with positive and negative values can also be partially reproduced. In particular, there are negative rates of period change for the calculated modes from our optimal model, which is not found in previous work.

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The rate of period change in DAV stars

Cited by 2 publications

References 72 publications

Probing the dark matter-electron interactions via hydrogen-atmosphere pulsating white dwarfs

Probing the dark matter-electron interactions via hydrogen-atmosphere pulsating white dwarfs

Asteroseismology of the DOV star PG 1159−035

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