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Hola. Dos preguntas.
1) He detectado algunas similitudes abajo mostradas. ¿podrían ser plagios?
2) Si, aparte de los mencionados abajo, también hay más supuestos plagios a un arxiv mio (con fecha obviamente anterior), y mi arxiv actualmente está enviado a un journal...¿deberían suspender la revisión de mi submision?
La lista es:
[FONT=&]1)[/FONT]
https://arxiv.org/pdf/1708.00407.pdf
[FONT=&]of relevant cases, such as the Einstein-Maxwell [21] and Einstein-Klein-Gordon system [22, 23, 24, 25], for higher derivative gravity [26, 27, 28], f(R)-theories of gravity [29, 30, 31, 32, 33, 34, 35], Hoˇrava-aether gravity [36, 37], polytropic spheres [38, 39, 40], among many others. In this respect, the simplest practical application of the MGD-decoupling consists in extending known isotropic and physically acceptable interior solutions for spherically symmetric self-gravitating systems into the anisotropic domain, at the same time preserving physical acceptability, which represents a highly non-trivial problem [41] (for obtaining anisotropic solutions in a generic way, see for instance Ref. [42, 43, 44]).[/FONT]
https://link.springer.com/article/10.1140/epjp/i2018-12074-2
[FONT=&]relevant cases, such as the Einstein-Maxwell [35] and Einstein-Klein-Gordon system [36–39], for higher derivative gravity [40,41], f(R) theories of gravity [42–48], Hoˇrava-aether gravity [49–51], and polytropic spheres [52–54]. In this respect, the simplest practical application of the MGD decoupling consists in extending known isotropic and physically acceptable interior solutions for spherically symmetric self-gravitating systems into the anisotropic domain, at the same time preserving physical acceptability, which is a highly non-trivial problem [55]. For obtaining anisotropic solutions in a generic way, see refs. [56,57][/FONT]
[FONT=&]2)[/FONT]
https://arxiv.org/pdf/1708.00407.pdf
[FONT=&]By using the MGD-decoupling approach, we presented in detail how to extend interior isotropic solutions for self-gravitating systems in order to include anisotropic (but still spherically symmetric) gravitational sources. For this purpose, we showed that the Einstein field equations for a static and spherically symmetric self-gravitating system in Eq. (2.6)-(2.8) can be decoupled in two sectors, namely: the isotropic sector corresponding to a perfect fluid Tˆ µν shown in Eq. (3.8)-(3.10), and the sector described by quasi-Einstein field equations associated with an anisotropic source θµν shown in Eqs. (3.12)-(3.14). These two sectors must interact only gravitationally, without direct exchange of energy-momentum.[/FONT]
https://link.springer.com/article/10.1140/epjp/i2018-12074-2
[FONT=&]Using the MGD decoupling, it was shown in detail how to extend an interior isotropic solution for a static and spherically symmetric self-gravitating system in order to include an additional gravitational source. For this purpose, it was shown that the Einstein’s field equations in eqs. (6)–(8) can be decoupled in a sector for a perfect fluid Ψ(m) μν shown in eqs. (13)–(15), and the sector describe by the equations associated with the additional gravitational source Φμν shown in eqs. (16)–(18). There is only gravitational interacction between these two sectors, and there is not exchange of energy momentum between them.[/FONT]
[FONT=&]3) [/FONT]https://arxiv.org/pdf/1708.00407.pdf
[FONT=&]The matching conditions at the stellar surface were then studied in detail for an outer Schwarzschild space-time. In particular, the continuity of the second fundamental form in Eq. (4.15) 16 was shown to yield the important result that the effective radial pressure ˜pR = 0. The effective pressure (2.11) contains both the isotropic pressure of the undeformed matter source Tˆ µν and the inner geometric deformation f ∗ (r) induced by the energy-momentum θµν.[/FONT]
https://link.springer.com/article/10.1140/epjp/i2018-12074-2
[FONT=&]The matching conditions at the star surface have been studied in detail for an outer Schwarzschild space-time. In particular, the continuity of the second fundamental form in eq. (28) yields the important result that the effective radial pressure ˜pR = 0. The effective pressure contains both the isotropic pressure of the gravitational source Ψ(m) μν and the geometric deformation η(r) induced by the energy-momentum tensor Φμν.
4) [/FONT]https://doi.org/10.1140/epjp/i2018-12074-2[FONT=&] :[/FONT]
[FONT=&]“Ruderman [7] about more realistic stellar models show that the nuclear matter may be anisotropic at least in certain very high density ranges (ρ > 1017 kg/m3), where the nuclear interactions must be treated relativistically”[/FONT]
otro preprint https://arxiv.org/abs/1805.00592 , fecha 2-5 dice:
Also the studies of Ruderman about more realistic stellar models show that the nuclear matter may be anisotropic at least in certain very high density ranges (ρ > 1015g/cm3), where the nuclear interactions must treated relativistically [5].
1) He detectado algunas similitudes abajo mostradas. ¿podrían ser plagios?
2) Si, aparte de los mencionados abajo, también hay más supuestos plagios a un arxiv mio (con fecha obviamente anterior), y mi arxiv actualmente está enviado a un journal...¿deberían suspender la revisión de mi submision?
La lista es:
[FONT=&]1)[/FONT]
https://arxiv.org/pdf/1708.00407.pdf
[FONT=&]of relevant cases, such as the Einstein-Maxwell [21] and Einstein-Klein-Gordon system [22, 23, 24, 25], for higher derivative gravity [26, 27, 28], f(R)-theories of gravity [29, 30, 31, 32, 33, 34, 35], Hoˇrava-aether gravity [36, 37], polytropic spheres [38, 39, 40], among many others. In this respect, the simplest practical application of the MGD-decoupling consists in extending known isotropic and physically acceptable interior solutions for spherically symmetric self-gravitating systems into the anisotropic domain, at the same time preserving physical acceptability, which represents a highly non-trivial problem [41] (for obtaining anisotropic solutions in a generic way, see for instance Ref. [42, 43, 44]).[/FONT]
https://link.springer.com/article/10.1140/epjp/i2018-12074-2
[FONT=&]relevant cases, such as the Einstein-Maxwell [35] and Einstein-Klein-Gordon system [36–39], for higher derivative gravity [40,41], f(R) theories of gravity [42–48], Hoˇrava-aether gravity [49–51], and polytropic spheres [52–54]. In this respect, the simplest practical application of the MGD decoupling consists in extending known isotropic and physically acceptable interior solutions for spherically symmetric self-gravitating systems into the anisotropic domain, at the same time preserving physical acceptability, which is a highly non-trivial problem [55]. For obtaining anisotropic solutions in a generic way, see refs. [56,57][/FONT]
[FONT=&]2)[/FONT]
https://arxiv.org/pdf/1708.00407.pdf
[FONT=&]By using the MGD-decoupling approach, we presented in detail how to extend interior isotropic solutions for self-gravitating systems in order to include anisotropic (but still spherically symmetric) gravitational sources. For this purpose, we showed that the Einstein field equations for a static and spherically symmetric self-gravitating system in Eq. (2.6)-(2.8) can be decoupled in two sectors, namely: the isotropic sector corresponding to a perfect fluid Tˆ µν shown in Eq. (3.8)-(3.10), and the sector described by quasi-Einstein field equations associated with an anisotropic source θµν shown in Eqs. (3.12)-(3.14). These two sectors must interact only gravitationally, without direct exchange of energy-momentum.[/FONT]
https://link.springer.com/article/10.1140/epjp/i2018-12074-2
[FONT=&]Using the MGD decoupling, it was shown in detail how to extend an interior isotropic solution for a static and spherically symmetric self-gravitating system in order to include an additional gravitational source. For this purpose, it was shown that the Einstein’s field equations in eqs. (6)–(8) can be decoupled in a sector for a perfect fluid Ψ(m) μν shown in eqs. (13)–(15), and the sector describe by the equations associated with the additional gravitational source Φμν shown in eqs. (16)–(18). There is only gravitational interacction between these two sectors, and there is not exchange of energy momentum between them.[/FONT]
[FONT=&]3) [/FONT]https://arxiv.org/pdf/1708.00407.pdf
[FONT=&]The matching conditions at the stellar surface were then studied in detail for an outer Schwarzschild space-time. In particular, the continuity of the second fundamental form in Eq. (4.15) 16 was shown to yield the important result that the effective radial pressure ˜pR = 0. The effective pressure (2.11) contains both the isotropic pressure of the undeformed matter source Tˆ µν and the inner geometric deformation f ∗ (r) induced by the energy-momentum θµν.[/FONT]
https://link.springer.com/article/10.1140/epjp/i2018-12074-2
[FONT=&]The matching conditions at the star surface have been studied in detail for an outer Schwarzschild space-time. In particular, the continuity of the second fundamental form in eq. (28) yields the important result that the effective radial pressure ˜pR = 0. The effective pressure contains both the isotropic pressure of the gravitational source Ψ(m) μν and the geometric deformation η(r) induced by the energy-momentum tensor Φμν.
4) [/FONT]https://doi.org/10.1140/epjp/i2018-12074-2[FONT=&] :[/FONT]
[FONT=&]“Ruderman [7] about more realistic stellar models show that the nuclear matter may be anisotropic at least in certain very high density ranges (ρ > 1017 kg/m3), where the nuclear interactions must be treated relativistically”[/FONT]
otro preprint https://arxiv.org/abs/1805.00592 , fecha 2-5 dice:
Also the studies of Ruderman about more realistic stellar models show that the nuclear matter may be anisotropic at least in certain very high density ranges (ρ > 1015g/cm3), where the nuclear interactions must treated relativistically [5].
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