Close-in Exoplanets as Candidates for Strange Quark Matter Objects
Close-in Exoplanets as Candidates for Strange Quark Matter Objects
复制标题
近距离系外行星是奇怪夸克物质天体的候选者
DOI：
10.3847/1538-4357/ab698b
复制
发表时间：
2019-08
影响因子：
4.9
通讯作者：
Gong Hang
中科院分区：
文献类型：
--
作者：
Kuerban Abudushataer;Geng Jin-Jun;Huang Yong-Feng;Zong Hong-Shi;Gong Hang
由于强子的真正基态可能是奇怪的夸克物质(SQM)，脉冲星实际上可能是奇怪的恒星，而不是中子星。根据这一SQM假说，奇异行星也可以稳定存在。正常物质行星的密度很难高于30g cm−3。当轨道半径小于5 6×10 10 cm或轨道周期(PORB)小于∼6 10 0 S时，它们将被潮汐破坏。然而，由于∼行星的高密度，它即使在离宿主非常近的情况下也可以安全地生存。此功能可以帮助我们识别SQM对象。在这里，我们试图在围绕脉冲星运行的近距离系外行星中寻找SQM天体。发现四颗脉冲星行星(XTE J1807-294b，XTE J1751-305b，PSR0636b，PSRJ1807-2459Ab)完全符合Porb<；6100 S的判据，因此是很好的SQM行星候选者。另外两颗行星(PSRJ1719-14b和PSRJ2051-0827b)的周期仅略大于准则值。他们可以被视为潜在的候选人。此外，我们还发现5颗白矮星(GP Com b、V396Hya b、J1433b、WD0137-349b和SDSS J1411+2009b)的周期都小于0.1天，它们也可能是SQM行星。从各种引力波探测器的角度计算了这些近距离行星系统的引力波发射。
Since the true ground state of hadrons may be strange quark matter (SQM), pulsars may actually be strange stars rather than neutron stars. According to this SQM hypothesis, strange planets can also stably exist. The density of normal matter planets can hardly be higher than 30 g cm−3. They will be tidally disrupted when the orbital radius is less than ∼5.6 × 1010 cm, or when the orbital period (Porb) is less than ∼6100 s. However, an SQM planet can safely survive even when it is very close to the host, due to its high density. This feature can help us identify SQM objects. Here, we have tried to search for SQM objects among close-in exoplanets orbiting around pulsars. It is found that four pulsar planets (XTE J1807-294 b, XTE J1751-305 b, PSR 0636 b, PSR J1807-2459A b) completely meet the criterion of Porb < 6100 s, and are thus good candidates for SQM planets. The periods of two other planets (PSR J1719-14 b and PSR J2051-0827 b) are only slightly larger than the criterion value. They could be regarded as potential candidates. Additionally, we find that the periods of five white dwarf planets (GP Com b, V396 Hya b, J1433 b, WD 0137-349 b, and SDSS J1411+2009 b) are less than 0.1 day; they might also be SQM planets. Gravitational wave emissions from these close-in planetary systems are calculated from the view of various gravitational wave detectors.
登录
查看更多内容
DOI：
10.1086/592743
发表时间：
2008-05
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
K. Lewis;P. Sackett;Rosemary A. Mardling School of Mathematical Sciences-Rosemary-A.-Mardling-School-of-Mathematical-102399213;Monash University;R. S. O. Astronomy;Astrophysics
通讯作者：
K. Lewis;P. Sackett;Rosemary A. Mardling School of Mathematical Sciences-Rosemary-A.-Mardling-School-of-Mathematical-102399213;Monash University;R. S. O. Astronomy;Astrophysics
影响因子：
3.5
作者：
J. Wright;Onsi Fakhouri;G. Marcy;E. Han;Ying Feng;J. Johnson;A. Howard;D. Fischer;J. Valenti-J.-V
通讯作者：
J. Wright;Onsi Fakhouri;G. Marcy;E. Han;Ying Feng;J. Johnson;A. Howard;D. Fischer;J. Valenti-J.-V
影响因子：
5
作者：
M. Shibata;E. Zhou;K. Kiuchi;S. Fujibayashi
通讯作者：
M. Shibata;E. Zhou;K. Kiuchi;S. Fujibayashi
影响因子：
3.5
作者：
R. Xu;G. J. Q. D. O. Geophysics;Peking University;Beijing;P. China;Ccast;P. R.China;CAS-PKU Joint Beijing Astrophysics Center
通讯作者：
R. Xu;G. J. Q. D. O. Geophysics;Peking University;Beijing;P. China;Ccast;P. R.China;CAS-PKU Joint Beijing Astrophysics Center
DOI：
10.1111/j.1365-2966.2011.18464.x
发表时间：
2011-02
期刊：
arXiv: High Energy Astrophysical Phenomena
影响因子：
--
作者：
M. Keith;S. Johnston;P. Ray;E. Ferrara;P. Parkinson;O. Celik;A. Belfiore;D. Donato;C. C. Cheung-C.;A. Abdo;F. Camilo;P. Freire;L. Guillemot;A. Harding;M. Kramer;P. Michelson;S. Ransom;R. Romani;D. Smith;D. Thompson;P. Weltevrede;K. Wood
通讯作者：
M. Keith;S. Johnston;P. Ray;E. Ferrara;P. Parkinson;O. Celik;A. Belfiore;D. Donato;C. C. Cheung-C.;A. Abdo;F. Camilo;P. Freire;L. Guillemot;A. Harding;M. Kramer;P. Michelson;S. Ransom;R. Romani;D. Smith;D. Thompson;P. Weltevrede;K. Wood