Neutron star solutions in perturbative quadratic gravity

Cemsinan Deliduman*, K. Y. Ekşi, Vildan Keleş

*Bu çalışma için yazışmadan sorumlu yazar

Araştırma sonucu: Dergiye katkıMakalebilirkişi

27 Atıf (Scopus)

Özet

We study the structure of neutron stars in R+βR μνR μν gravity model with perturbative method. We obtain mass-radius relations for six representative equations of state (EoSs). We find that, for |β| ∼ 10 11 cm 2, the results differ substantially from the results of general relativity. Some of the soft EoSs that are excluded within the framework of general relativity can be reconciled for certain values of β of this order with the 2 solar mass neutron star recently observed. For values of β greater than a few 10 11 cm 2 we find a new solution branch allowing highly massive neutron stars. By referring some recent observational constraints on the mass-radius relation we try to constrain the value of β for each EoS. The associated length scale (β) 1/2 ∼ 10 6 cm is of the order of the the typical radius of neutron stars, the probe used in this test. This implies that the true value of β is most likely much smaller than 10 11 cm 2.

Orijinal dilİngilizce
Makale numarası036
DergiJournal of Cosmology and Astroparticle Physics
Hacim2012
Basın numarası5
DOI'lar
Yayın durumuYayınlandı - May 2012

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