First Asteroseismic Limits on the Nature of Dark Matter

Casanellas, Jordi; Lopes, Ilídio

doi:10.1088/2041-8205/765/1/l21

Cited by 50 publications

(69 citation statements)

References 51 publications

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“…Casanellas and Lopes [20] suggested that the use of diagnostics from stellar oscillations could be used to constrain the properties of DM. In a follow-up, Casanellas and Lopes [21] reported the first asteroseismic constraints for WIMP-like ADM from solar-like stars.…”

Section: Introductionmentioning

confidence: 95%

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Asteroseismic constraints on asymmetric dark matter: Light particles with an effective spin-dependent coupling

2017

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So far, direct detection searches have come empty handed in their quest for Dark Matter (DM). Meanwhile, asteroseismology arises as a complementary tool to study DM, as its accumulation in a star can enhance energy transport, by providing a conduction mechanism, producing significant changes in the stellar structure during the course of the star's evolution. The stellar core, particularly affected by the presence of DM, can be investigated through precise asteroseismic diagnostics. We modelled three stars including DM energy transport: the Sun, a slightly less massive and much older star, KIC 7871531 (0.85 M ⊙ , 9.41 Gyr), and a more massive and younger one, KIC 8379927 (1.12 M ⊙ , 1.82 Gyr). We considered both the case of Weakly Interactive Massive Particles, albeit with a low annihilation, and the case of Asymmetric DM for which the number of trapped particles in the star can be much greater. By analysing these models with asteroseismic separation ratios weighted towards the core, we found indications limiting the effective spin-dependent DM-proton coupling for masses of a few GeV. This independent result is very close to the most recent and most stringent direct detection DM constraints.

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Section: Introductionmentioning

confidence: 95%

“…Asteroseismology has been used before to study the effects of WIMP-like ADM in stars less massive than the Sun [21]. However, this is the first time that asteroseismic signatures of a star less massive than the Sun are used to study self-interacting ADM, hereafter known simply as ADM.…”

Section: Introductionmentioning

confidence: 99%

Asteroseismic constraints on asymmetric dark matter: Light particles with an effective spin-dependent coupling

2017

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“…Although the density of DM in our region of the Galaxy is estimated to be very low, ρ χ ≈ 0.4 GeV cm −3 [15], it suffices to change the internal properties of stars similar to the Sun [5]. In environments with greater DM densities, such as the center of the Milky Way and inside dwarf galaxies and globular clusters, the impact on stars could be much larger [16][17][18][19], in particular in the case of compact stars [20,21].…”

Section: Impact Of Dark Matter On Starsmentioning

confidence: 89%

“…In fact, one of the reasons for WIMPs to be very popular DM candidates is that their existence could be detected in ongoing or upcoming experiments [1]. Stellar physics and observations have provided fruitful insights in particle physics and cosmology [2,3], triggering advances in the understanding of neutrino interactions and oscillations [4], and setting bounds on new particles like WIMPs [5], axions [6] and other light bosons [7]. In this context, the unprecedented abundance of high-quality data from asteroseismic missions like CoRoT [8] and Kepler [9] opens up the possibility of further use the stars as laboratories for fundamental physics [10].…”

Section: Introductionmentioning

confidence: 99%

Dark matter searches with asteroseismology

Casanellas

2015

EPJ Web of Conferences

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Abstract. High-precision asteroseismic data provides an excellent opportunity to test theories of stellar evolution and new physics, such as the properties of the dark matter (DM) of the Universe. Here we will show that some models of DM lead to changes in the classical scenario of stellar evolution. The accumulation of DM in the core of low-mass stars reduces their central temperatures and inhibits the formation of small convective cores in 1.1-1.3 Ms stars. We review the asteroseismic constraints that have been set to the characteristics of the DM particles, obtained comparing the oscillations of the star α Cen B with modified stellar models. To conclude, we discuss the prospects to use CoRoT and Kepler data on main-sequence stars and red giants to further constrain the nature of DM.

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“…Moreover, it has been shown for the Solar data produced by the VIRGO (Fröhlich et al 1995) and GOLF (Gabriel et al 1995) experiments that the noise in the amplitude spectra caused by the variations produced by granulation in the photosphere of the star is much larger for the intensity measurements than for the radial velocities. If pulsations were to be discovered, it would deeply impact our understanding of M dwarfs and all related science, such as planet and star formation and evolution, galactic evolution or constraints on the parameters of dark matter (Casanellas & Lopes 2013). Discovery of pulsations will allow the application of asteroseismic methods to study M dwarf internal structure, providing, for instance, the mean density and the depth of the external convective layer.…”

Section: Discussionmentioning

confidence: 99%

M dwarf search for pulsations within Kepler Guest Observer programme

Rodríguez‐López

Gizis

MacDonald

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present the analysis of four M dwarf stars -plus one M giant that seeped past our selection criteria-observed in Cycle 3 of Kepler Guest Observer program (GO3) in a search for intrinsic pulsations. Stellar oscillations in M dwarfs were theoretically predicted by Rodríguez-López et al. (2012) to be in the range ∼20-40 min and ∼4-8 h, depending on the age and the excitation mechanism. We requested Kepler short cadence observations to have an adequate sampling of the oscillations. The targets were chosen on the basis of detectable rotation in the initial Kepler results, biasing towards youth.The analysis reveals no oscillations attributable to pulsations at a detection limit of several parts per million, showing that either the driving mechanisms are not efficient in developing the oscillations to observable amplitudes, or that if pulsations are driven, the amplitudes are very low. The size of the sample, and the possibility that the instability strip is not pure, allowing the coexistence of pulsators and non-pulsators, prevent us from deriving definite conclusions. Inmediate plans include more M dwarfs photometric observations of similar precision with Kepler K2 mission and spectroscopic searches already underway within the Cool Tiny Beats Project Berdiñas et al. 2014) with the high-resolution spectrographs HARPS and HARPS-N.

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First Asteroseismic Limits on the Nature of Dark Matter

Cited by 50 publications

References 51 publications

Asteroseismic constraints on asymmetric dark matter: Light particles with an effective spin-dependent coupling

Asteroseismic constraints on asymmetric dark matter: Light particles with an effective spin-dependent coupling

Dark matter searches with asteroseismology

M dwarf search for pulsations within Kepler Guest Observer programme

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