Bhatia - Hazarika Limit
Bhatia Hazarika limit is astronomical event that occurs on forming Black hole after the Gravitational collapse of a Neutron star attaining the size of 2.8 Solar mass,[1][2] ,.[3] Theoretically,[4][5][6],[7] ,[8],[9] , for rotating neutron star or Pulsar unlike
Tolman–Oppenheimer–Volkoff limit .
Which is for non-rotational neutron stars.
It is observed in GW170817 in LIGO that Gravitational wave of two Neutron star collision leading to Gravitational collapse with 2.8 Solar mass . It is observed in GW190814 also have 2.8 solar mass or more.
A neutron star smash breaks universe showing 2.8 Solar mass shown in a lecture at Niels Bohr Institute of University of Copenhagen.[10]
A book' 'Seeing god through science'' exploring the universe narrates that Gravitational collapse occurs at 2.8 Solar mass.[11] The complex life of star cluster of Neutron star is 2.8 times of Solar mass,.[12][13] NASA [14] the book " Extreme stars",.[15][16]
References[edit]
- ↑ Siegel, Ethan. "The Surprising Reason Why Neutron Stars Don't All Collapse To Form Black Holes". Forbes. Retrieved 2024-01-02.
- ↑ "Lecture 19: Neutron Stars". sites.ualberta.ca. Retrieved 2024-01-02.
- ↑ "Solution Set #6". www.aoc.nrao.edu. Retrieved 2024-01-02.
- ↑ Bhatia, P K; Hazarika, A B Rajib (1996-01-01). "Stability of two viscous rotating superposed gravitating streams in a uniform horizontal magnetic field". Physica Scripta. 53 (1): 57–61. Bibcode:1996PhyS...53...57B. doi:10.1088/0031-8949/53/1/011. ISSN 0031-8949. Unknown parameter
|s2cid=ignored (help) - ↑ "Solution Set #6". www.aoc.nrao.edu. Retrieved 2024-01-02.
- ↑ "What would be the effects of a neutron star if one was heading towards our solar system?". Quora. Retrieved 2024-01-02.
- ↑ "Bhatia Hazarika limitの意味・使い方・読み方 | Weblio英和辞書". ejje.weblio.jp. Retrieved 2024-01-03.
- ↑ Dewi, J. D. M.; Pols, O. R. (2003-09-01). "The late stages of evolution of helium star-neutron star binaries and the formation of double neutron star systems". Monthly Notices of the Royal Astronomical Society. 344 (2): 629–643. arXiv:astro-ph/0306066. Bibcode:2003MNRAS.344..629D. doi:10.1046/j.1365-8711.2003.06844.x. ISSN 0035-8711. Unknown parameter
|s2cid=ignored (help) - ↑ Abhyankar, K. D. (1991). "1991BASI...19..105A Page 105". Bulletin of the Astronomical Society of India. 19: 105. Bibcode:1991BASI...19..105A. Retrieved 2024-01-03.
- ↑ Toulouse, Corinne (2022-02-16). "Neutron star smash shakes universe". nbi.ku.dk. Retrieved 2024-01-02.
- ↑ Schoub, Barry David (2019-08-27). Seeing God Through Science: Exploring the Science Narrative to Strengthen and Deepen Faith in the Creator. Wipf and Stock Publishers. ISBN 978-1-5326-8712-9. Search this book on
- ↑ Stevenson, David (2015-05-09). The Complex Lives of Star Clusters. Springer. ISBN 978-3-319-14234-0. Search this book on
- ↑ Council, National Research; Applications, Commission on Physical Sciences, Mathematics, and; Board, Space Studies; Astronomy, Board on Physics and; Committee, Astronomy and Astrophysics Survey (2001-02-16). Astronomy and Astrophysics in the New Millennium. National Academies Press. ISBN 978-0-309-07031-7. Search this book on
- ↑ SVS (2010-01-26). "NASA Scientific Visualization Studio | Neutron Star Merge". SVS. Retrieved 2024-01-02.
- ↑ Kaler, James B. (2006-05-07). The Hundred Greatest Stars. Springer Science & Business Media. ISBN 978-0-387-21625-6. Search this book on
- ↑ Kaler, James B. (2001-03-22). Extreme Stars: At the Edge of Creation. Cambridge University Press. ISBN 978-0-521-40262-0. Search this book on
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