Stella neutronica

Stella neutronica est nucleus collapsus supergigantis, cuius prior erat massa inter 10 et 25 massarum solarium, vel fortasse grandior si dives erat stella metallorum,^[1] qui factus est stella degener. Exceptis foraminibus nigris et aliquîs corporibus hypotheticis (e.g. foraminibus albis, stellis quarcicis), stellae neutronicae sunt minimae et densissimae corporum stellarum.^[2] Radium habent ordine 10 chiliometrorum et massam circiter 1.4 massarum solarium.^[3] Coniunctio explosionis supergigantis cum collapsione gravitationali – quae nucleum stellarem plus quam ad densitatem pumilionum albarum et usque ad densitatem nucleorum atomicorum comprimit – stellam neutronicam gignit.

Post quam stellae neutronicae creantur non alium calorem generant et lente refrigerant; possunt tamen ultro per collisiones vel accretionem evolvere. Pleraque coniectationes de his corporibus inferunt stellas neutronicas paene omnino neutronibus constare (particulis subatomicis nullo onere electrico et massa paulo grandiore quam massa protonis). Nam electrones materiei vulgaris cum protonibus extremo regimine stellarum neutronicarum miscentur ut neutrones generent.

Stellae neutronicae contra ulteriorem contrationem pressione degenerationis neutronum sustinentur (effectu exclusionis principio Pauli appellato) sicut pressio degenerationis electronum pumiliones albas sustinet. Per se non sufficit tamen talis pressio ut stellam sustineat ultra 0.7 M_☉,^[4]^[5] et repulsivae vires nucleares maxime interveniunt ad stellas neutronicas grandiores sustinendas.^[6]^[7] Si massa stellae excedit limitem Tolman–Oppenheimer–Volkoff duarum massarum solarium, aequabilitas pressionis et virium nuclearum insufficiens fit, et stella tum collabitur adusque foramen nigrum creatur. Stella neutronica maxima massa detecta, PSR J0952–0607, aestimatur 2.35 ± 0.17 massis solaribus.^[8]

Genesis

Stella, quae plus quam sesqualterum (exacte: 1,4) massae Solis nostri habet, cum paene omne plasma metallorum in ferri plasma mutavisset, sphaeris externis amissis contrahitur. Massa autem stellae tanta est ut electrones et protona non iam libere esse possint, sed coeant ita ut neutrona existant neutrinaque emittantur. Quae actio beta dissolutio inversa vocatur.

Si quidem massa stellae plus quam triplum (exacte 3.2) massae Solis est, aliud obiectum fit foramen nigrum. Stellae minoris massae autem pumiliones albae fiunt.

Qualitates

Stella neutronica usualis circiter sesqualtera massa Solis habet, diametrum autem modo viginti chiliometrûm. Superficies frigida est,^{citatio desiderata} sine ulla pressione atmosphaerica. Beta dissolutionis causa non e neutronibus constat, sed ferrea est, quia ferro nucleus maxime stabilis est.

In interiore autem materia e neutronibus constat, quae materia ibi quasi fluida est.

Si stella gravior est, in imo neutrona in quarcia dissolvi possint: Hae stellae hypotheticae stellae insolentae vocantur.

Stellae neutronicae radios et lucis et roentgenios emittere solent, et celerrime circum axem suam rotantur. Radii roentgenii si quasi in lineam conferti emittuntur, stella pulsar appellatur; nam haec linea radiorum propter rotationem stellae ad nos non nisi pulsata pervenit.

Nexus interni

Notae

↑ Heger, A.; Fryer, C. L.; Woosley, S. E.; Langer, N.; Hartmann, D. H. (2003). "How Massive Single Stars End Their Life". Astrophysical Journal 591 (1): 288–300. arXiv:astro-ph/0212469
↑ Glendenning, Norman K. (2012). Compact Stars: Nuclear Physics, Particle Physics and General Relativity (illustrated ed.). Springer Science & Business Media. p. 1. ISBN 978-1-4684-0491-3
↑ Seeds, Michael; Backman, Dana (2009). Astronomy: The Solar System and Beyond (6th ed.). Cengage Learning. p. 339. ISBN 978-0-495-56203-0
↑ Tolman, R. C. (1939). "Static Solutions of Einstein's Field Equations for Spheres of Fluid". Physical Review 55 (4): 364–373
↑ Oppenheimer, J. R.; Volkoff, G. M. (1939). "On Massive Neutron Cores". Physical Review 55 (4): 374–381
↑ Neutron Stars. . www.astro.princeton.edu
↑ Douchin, F.; Haensel, P. (December 2001). "A unified equation of state of dense matter and neutron star structure". Astronomy & Astrophysics 380 (1): 151–167. arXiv:astro-ph/0111092
↑ "The heaviest neutron star on record is 2.35 times the mass of the sun". sciencenews. 22 July 2022

[1] Heger, A.; Fryer, C. L.; Woosley, S. E.; Langer, N.; Hartmann, D. H. (2003). "How Massive Single Stars End Their Life". Astrophysical Journal 591 (1): 288–300. arXiv:astro-ph/0212469

[2] Glendenning, Norman K. (2012). Compact Stars: Nuclear Physics, Particle Physics and General Relativity (illustrated ed.). Springer Science & Business Media. p. 1. ISBN 978-1-4684-0491-3

[3] Seeds, Michael; Backman, Dana (2009). Astronomy: The Solar System and Beyond (6th ed.). Cengage Learning. p. 339. ISBN 978-0-495-56203-0

[4] Tolman, R. C. (1939). "Static Solutions of Einstein's Field Equations for Spheres of Fluid". Physical Review 55 (4): 364–373

[5] Oppenheimer, J. R.; Volkoff, G. M. (1939). "On Massive Neutron Cores". Physical Review 55 (4): 374–381

[6] Neutron Stars. . www.astro.princeton.edu

[7] Douchin, F.; Haensel, P. (December 2001). "A unified equation of state of dense matter and neutron star structure". Astronomy & Astrophysics 380 (1): 151–167. arXiv:astro-ph/0111092

[8] "The heaviest neutron star on record is 2.35 times the mass of the sun". sciencenews. 22 July 2022

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