Bosonic dark matter in neutron stars and its effect on gravitational wave signal

Karkevandi, Davood Rafiei; Shakeri, Soroush; Sagun, V. V.; Ivanytskyi, O.

doi:10.1103/physrevd.105.023001

Cited by 85 publications

(77 citation statements)

References 167 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We expect that future improved measurements coming from next-generation gravitational interferometers will be able to utilize this observable to assess the DM content of merging compact stars, as emphasized in Refs. [34,37,56,57,60].…”

Section: Discussionmentioning

confidence: 99%

“…[58,59], and for a mixture of bosonic DM and neutron star matter in Refs. [34,37]. Note that Ellis et al in Ref.…”

Section: Introductionmentioning

confidence: 93%

“…At the same time, self-annihilating DM accreted onto neutron stars may significantly change their kinematical properties [19] or provide a mechanism to seed compact objects with longlived lumps of strangelets [20]. Furthermore, neutron stars that accommodate non-self-annihilating DM have emerged as an interesting astrophysical scenario for analyzing the effects of DM on hadronic matter (or even quark matter) under extreme conditions [16,[21][22][23][24][25][26][27][28][29][30][31][32][33][34][35][36][37][38][39]. In this context, the existence of compact objects with Earth-or Jupiterlike masses but unusual small radii has been put forward [40][41][42], allowing for a new scenario to determine the existence and nature of DM.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Second Love number of dark compact planets and neutron stars with dark matter

2022

View full text Add to dashboard Cite

We study the mass-radius relation and the second Love number of compact objects made of ordinary matter and non-self-annihilating fermionic dark matter for a wide range of dark matter particle masses, and for the cases of weakly and strongly interacting dark matter. We obtain stable configurations of compact objects with radii smaller than 10 km and masses similar to Earth-or Jupiter-like stellar objects. In certain parameter ranges, we find second Love numbers which are markedly different compared to those expected for neutron stars without dark matter. Thus, by obtaining the compactness of these compact objects and measuring their tidal deformability from gravitational wave detections from binary neutron star mergers, the extracted value of the second Love number would allow us to determine the existence of dark matter inside neutron stars irrespective of the equation of state of ordinary matter.

show abstract

Section: Discussionmentioning

confidence: 99%

“…[58,59], and for a mixture of bosonic DM and neutron star matter in Refs. [34,37]. Note that Ellis et al in Ref.…”

Section: Introductionmentioning

confidence: 93%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Second Love number of dark compact planets and neutron stars with dark matter

2022

View full text Add to dashboard Cite

show abstract

“…Moreover, new observables can appear in NS mergers, such as additional peaks in the postmerger frequency spectrum [487], and the tidal deformability (Λ) can decrease (increase) in the case of dark cores [32] (halos [488]); see also Ref. [489]. Moreover, the DM content of an NS can impact its EoS, so that, e.g., an EoS that was ruled out from the GW observation of the upper bound on Λ could be revived if a small admixture, say 5%, of DM were present.…”

Section: Other Imprints Of Dm Physics On Nss and Their Mergersmentioning

confidence: 99%

Neutron Stars with Baryon Number Violation, Probing Dark Sectors

2022

View full text Add to dashboard Cite

The neutron lifetime anomaly has been used to motivate the introduction of new physics with hidden-sector particles coupled to baryon number, and on which neutron stars provide powerful constraints. Although the neutron lifetime anomaly may eventually prove to be of mundane origin, we use it as motivation for a broader review of the ways that baryon number violation, be it real or apparent, and dark sectors can intertwine and how neutron star observables, both present and future, can constrain them.

show abstract

“…The effects of bosonic DM on the gravitational wave signals were studied in Ref. [55]. In our recent works [38,56], we considered the fermionic DM, which interacts with nucleons via the Higgs mechanism.…”

Section: Introductionmentioning

confidence: 99%

Dark Matter Effects on the Compact Star Properties

Das

Kumar

et al. 2022

Galaxies

View full text Add to dashboard Cite

The neutron star properties are generally determined by the equation of state of β-equilibrated dense matter. In this work, we consider the interaction of fermionic dark matter (DM) particles with nucleons via Higgs exchange and investigate the effect on the neutron star properties with the relativistic mean-field model equation of state coupled with DM. We deduce that DM significantly affects the neutron star properties, such as considerably reducing the maximum mass of the star, which depends on the percentage of the DM considered inside the neutron star. The tidal Love numbers both for electric and magnetic cases and surficial Love numbers are also studied for DM admixed NS. We observed that the magnitude of tidal and surficial Love numbers increases with a greater DM percentage. Further, we present post-Newtonian tidal corrections to gravitational waves decreased by increasing the DM percentage. The DM effect on the GW signal is significant during the late inspiral and merger stages of binary evolution for GW frequencies >500 Hz.

show abstract

Bosonic dark matter in neutron stars and its effect on gravitational wave signal

Cited by 85 publications

References 167 publications

Second Love number of dark compact planets and neutron stars with dark matter

Second Love number of dark compact planets and neutron stars with dark matter

Neutron Stars with Baryon Number Violation, Probing Dark Sectors

Dark Matter Effects on the Compact Star Properties

Contact Info

Product

Resources

About