Study on charged strange stars in f(R, T) gravity; Journal of Cosmology and Astroparticle Physics; Vol. 2019
| Parent link: | Journal of Cosmology and Astroparticle Physics Vol. 2019.— 2019.— [27 p.] |
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| Erakunde egilea: | |
| Beste egile batzuk: | , , , |
| Gaia: | Title screen We investigate the effects of the modified f(R, T) gravity on the charged strange quark stars with the standard choice of f(R, T)=R+2χ T. Those types of stars are supposed to be made of strange quark matter (SQM) whose distribution is governed by the phenomenological MIT bag EOS as p=1/3(ρ−4B), where B is the bag constant, while the form of charge distribution is chosen to be q(r)=Q(r/)3=α r3 with α as a constant. We derive the values of the unknown parameters by matching the interior spacetime to the exterior Reissner-Nordstr{öm metric followed by the appropriate choice of the values of the parameters χ and α. Our study reveals that besides SQM, a new kind of matter distribution originates due to the interaction between the matter and the extra geometric term, while the modification of the Tolman-Oppenheimer-Volkoff (TOV) equation invokes the presence of a new force Fc. The accumulation of the electric charge distribution reaches its maximum at the surface, and the predicted values of the corresponding electric charge and electric field are of the order of 1019−20C and 1021−22 V/cm, respectively. To examine the physical validity of our solutions, we perform tests of the energy conditions, stability against the equilibrium of the forces, the adiabatic index, etc., and find that the proposed f(R, T) model survives all these critical tests. Therefore, our model can describe the non-singular charged strange stars and justify the supermassive compact stellar objects having their masses beyond the maximum mass limit for the compact stars in the standard scenario. Our model also supports the existence of several exotic astrophysical objects like super-Chandrasekhar white dwarfs, massive pulsars, and even magnetars, which remain unexplained in the framework of General Relativity (GR). Режим доступа: по договору с организацией-держателем ресурса |
| Hizkuntza: | ingelesa |
| Argitaratua: |
2019
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| Gaiak: | |
| Sarrera elektronikoa: | http://dx.doi.org/10.1088/1475-7516/2019/10/070 |
| Formatua: | Baliabide elektronikoa Liburu kapitulua |
| KOHA link: | https://koha.lib.tpu.ru/cgi-bin/koha/opac-detail.pl?biblionumber=662053 |
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| 200 | 1 | |a Study on charged strange stars in f(R, T) gravity |f D. Deb, S. V. Ketov, M. Yu. Khlopov, S. Ray | |
| 203 | |a Text |c electronic | ||
| 300 | |a Title screen | ||
| 320 | |a [References: 129 tit.] | ||
| 330 | |a We investigate the effects of the modified f(R, T) gravity on the charged strange quark stars with the standard choice of f(R, T)=R+2χ T. Those types of stars are supposed to be made of strange quark matter (SQM) whose distribution is governed by the phenomenological MIT bag EOS as p=1/3(ρ−4B), where B is the bag constant, while the form of charge distribution is chosen to be q(r)=Q(r/)3=α r3 with α as a constant. We derive the values of the unknown parameters by matching the interior spacetime to the exterior Reissner-Nordstr{öm metric followed by the appropriate choice of the values of the parameters χ and α. Our study reveals that besides SQM, a new kind of matter distribution originates due to the interaction between the matter and the extra geometric term, while the modification of the Tolman-Oppenheimer-Volkoff (TOV) equation invokes the presence of a new force Fc. The accumulation of the electric charge distribution reaches its maximum at the surface, and the predicted values of the corresponding electric charge and electric field are of the order of 1019−20C and 1021−22 V/cm, respectively. To examine the physical validity of our solutions, we perform tests of the energy conditions, stability against the equilibrium of the forces, the adiabatic index, etc., and find that the proposed f(R, T) model survives all these critical tests. Therefore, our model can describe the non-singular charged strange stars and justify the supermassive compact stellar objects having their masses beyond the maximum mass limit for the compact stars in the standard scenario. Our model also supports the existence of several exotic astrophysical objects like super-Chandrasekhar white dwarfs, massive pulsars, and even magnetars, which remain unexplained in the framework of General Relativity (GR). | ||
| 333 | |a Режим доступа: по договору с организацией-держателем ресурса | ||
| 461 | |t Journal of Cosmology and Astroparticle Physics | ||
| 463 | |t Vol. 2019 |v [27 p.] |d 2019 | ||
| 610 | 1 | |a электронный ресурс | |
| 610 | 1 | |a труды учёных ТПУ | |
| 610 | 1 | |a dark energy theory | |
| 610 | 1 | |a massive stars | |
| 610 | 1 | |a modified gravity | |
| 610 | 1 | |a темная энергия | |
| 610 | 1 | |a массивные звезды | |
| 610 | 1 | |a модифицированная гравитация | |
| 701 | 1 | |a Deb |b D. |g Debabrata | |
| 701 | 1 | |a Ketov |b S. V. |c physicist |c Professor of Tomsk Polytechnic University, Doctor of physical and mathematical sciences |f 1960- |g Sergey Vladimirovich |3 (RuTPU)RU\TPU\pers\36631 |9 19672 | |
| 701 | 1 | |a Khlopov |b M. Yu. |g Maksim Yurjevich | |
| 701 | 1 | |a Ray |b S. |g Saibal | |
| 712 | 0 | 2 | |a Национальный исследовательский Томский политехнический университет |b Исследовательская школа физики высокоэнергетических процессов |c (2017- ) |3 (RuTPU)RU\TPU\col\23551 |
| 801 | 1 | |a RU |b 63413507 |c 20140916 | |
| 801 | 2 | |a RU |b 63413507 |c 20200513 |g RCR | |
| 850 | |a 63413507 | ||
| 856 | 4 | |u http://dx.doi.org/10.1088/1475-7516/2019/10/070 | |
| 942 | |c CF | ||