Kilonova

kilonova (wanda kuma ake kira macronova) wani lamari ne na astronomical wanda ke faruwa a cikin tsarin binary mai mahimmanci lokacin da taurari biyu na neutron ko tauraron neutron da ramin baki suka haɗu. Wadannan haɗuwa ana zaton suna samar da fashewar (gamma-ray) kuma suna fitar da radiation mai haske na lantarki, wanda ake kira "kilonovae", saboda lalacewar rediyo na tsananin r-process da aka samar kuma aka fitar da su daidai a lokacin haɗuwa.An ƙaddamar da girman ƙirar kilonova AT2017gfo a farkon lokutan daga yanayin baƙar fata na bakanta.     

 Tarihi 
Li & Paczyński ne suka fara gabatar da kasancewar abubuwan da suka faru na yanayi daga haɗuwa da tauraron neutron a shekarar 1998. Li, L.-X.; Paczyński, B.; Fruchter, A. S.; Hjorth, J.; Hounsell, R. A.; Wiersema, K.; Tunnicliffe, R. (1998). "Transient Events from Neutron Star Mergers". The Astrophysical Journal. 507 (1): L59–L62. arXiv:astro-ph/9807272. Bibcode:1998ApJ...507L..59L. doi:10.1086/311680. S2CID 3091361. Hasken rediyo wanda ya samo asali daga haɗuwa da haɗuwa an kira shi da farko mini-supernova, saboda yana da  zuwa  hasken supernova na yau da kullun, fashewar kansa na babban tauraron.   Kalmar kilonova daga baya Metzger et al. ne suka gabatar da ita a cikin 2010  don nuna alamar haske, wanda suka nuna ya kai sau 1000 na nova na gargajiya.

An gano dan takarar farko da aka samu a ranar 3 ga Yuni, 2013 a matsayin ɗan gajeren gamma-ray fashewa GRB 130603B ta kayan aiki a cikin jirgin Swift Gamma-Ray Burst Explorer da KONUS / WIND, sannan kuma Hubble Space Telescope ya ɗauka 9 da 30 kwanaki bayan haka.
A ranar 16 ga Oktoba, 2017, haɗin gwiwar LIGO da Virgo sun ba da sanarwar ganowa ta farko ta raƙuman ruwa (GW170817 ) wanda zai dace da lura da wutar lantarki, kuma ya nuna cewa tushen ya Haɗuwa da tauraron neutron.  Wannan haɗuwa ta biyo bayan ɗan gajeren GRB (GRB 170817A) da kuma ɗan gajeren lokaci mai tsawo wanda ake gani na makonni a cikin bakan lantarki na gani da na kusa (AT 2017gfo), wanda ke da shekaru haske miliyan 140 kawai a cikin galaxy mai kusa NGC 4993. Binciken AT 2017gfo ya tabbatar da cewa shine farkon lura na kilonova.  Tsarin ƙira na AT2017gfo ya gano abubuwa na r-process strontium da yttrium, wanda ke da alaƙa da kafa abubuwa masu nauyi zuwa haɗuwa da neutron-star. Ƙarin ƙira ya nuna ƙwallon wuta da aka fitar na abubuwa masu nauyi ya kasance mai ƙwanƙwasawa sosai a farkon lokutan.Sneppen, Albert; Watson, Darach; Bauswein, Andreas; Just, Oliver; Kotak, Rubina; Nakar, Ehud; Poznanski, Dovi; Sim, Stuart (February 2023). "Spherical symmetry in the kilonova AT2017gfo/GW170817". Nature. 614 (7948): 436–439. arXiv:2302.06621. Bibcode:2023Natur.614..436S. doi:10.1038/s41586-022-05616-x. ISSN 1476-4687. PMID 36792736. S2CID 256846834. Wasu masu bincike sun ba da shawarar cewa "godiya ga wannan aikin, masu binciken sararin samaniya na iya amfani da kilonovae a matsayin kyandir mai ma'ana don auna fadada sararin samaniya. Tunda fashewar kilonovaes suna da siffar siffar siyarwa, masu binciken taurari na iya kwatanta girman fashewar supernova da ainihin girmansa kamar yadda aka gani ta hanyar motsi na gas, don haka auna yawan fadada sarkar samaniya a nesa daban-daban".

 Ka'idar 
Halitta da haɗuwa da abubuwa biyu masu mahimmanci sune tushen raƙuman ruwa (GW). Metzger, B. D.; Martínez-Pinedo, G.; Darbha, S.; Quataert, E.; Arcones, A.; Kasen, D.; Thomas, R.; Nugent, P.; Panov, I. V.; Zinner, N. T. (August 2010). "Electromagnetic counterparts of compact object mergers powered by the radioactive decay of r-process nuclei". Monthly Notices of the Royal Astronomical Society. 406 (4): 2650. arXiv:1001.5029. Bibcode:2010MNRAS.406.2650M. doi:10.1111/j.1365-2966.2010.16864.x. S2CID 118863104. Li-Xin Li da Bohdan Paczyński ne suka gabatar da samfurin asali don yanayin zafi daga haɗuwa da tauraron neutron a cikin 1998. Li, L.-X.; Paczyński, B.; Fruchter, A. S.; Hjorth, J.; Hounsell, R. A.; Wiersema, K.; Tunnicliffe, R. (1998). "Transient Events from Neutron Star Mergers". The Astrophysical Journal. 507 (1): L59–L62. arXiv:astro-ph/9807272. Bibcode:1998ApJ...507L..59L. doi:10.1086/311680. S2CID 3091361. A cikin aikinsu, sun ba da shawarar cewa fitar da rediyo daga haɗuwa da tauraron neutron shine tushen samar da wutar lantarki, daga baya aka kira kilonova.

 Abubuwan da aka lura 
Shawarwarin lura na farko na kilonova ya zo ne a cikin 2008 biyo bayan fashewar gamma-ray GRB 080503,  inda wani abu mai rauni ya bayyana a cikin haske na gani bayan kwana ɗaya kuma ya ɓace cikin sauri. Koyaya, wasu dalilai kamar rashin tauraron dan adam da gano X-ray ba su yarda da ra'ayin kilonova ba. An ba da shawarar wani kilonova a cikin 2013, tare da haɗin gwiwar ɗan gajeren lokaci na GRB 130603B, inda aka gano fitar da infrared mai sauƙi daga kilonova mai nisa ta amfani da Hubble Space Telescope.Tanvir, N. R.; Levan, A. J.; Fruchter, A. S.; Hjorth, J.; Hounsell, R. A.; Wiersema, K.; Tunnicliffe, R. L. (2013). "A 'kilonova' associated with the short-duration γ-ray burst GRB 130603B". Nature. 500 (7464): 547–549. arXiv:1306.4971. Bibcode:2013Natur.500..547T. doi:10.1038/nature12505. PMID 23912055. S2CID 205235329.

A watan Oktoba na shekara ta 2017, masu binciken taurari sun ba da rahoton cewa abubuwan da aka lura da AT 2017gfo sun nuna cewa shi ne karo na farko da aka samu na kilonova bayan hadewar taurari biyu na neutron.Abbott, B. P.; Abbott, R.; Abbott, T. D.; Acernese, F.; Ackley, K.; Adams, C.; Adams, T.; Addesso, P.; Adhikari, R. X.; Adya, V. B.; Affeldt, C.; Afrough, M.; Agarwal, B.; Agathos, M.; Agatsuma, K. (2017-10-16). "Multi-messenger Observations of a Binary Neutron Star Merger". The Astrophysical Journal. 848 (2): L12. arXiv:1710.05833. Bibcode:2017ApJ...848L..12A. doi:10.3847/2041-8213/aa91c9. ISSN 2041-8213. S2CID 217162243.
A watan Oktoba na shekara ta 2018, masu binciken taurari sun ba da rahoton cewa GRB 150101B, wani fashewar gamma-ray da aka gano a shekarar 2015, na iya zama kwatankwacin tarihin GW170817. Abubuwan da suka faru tsakanin abubuwan da suka faru guda biyu, dangane da hasken gamma, hasken ido da hasken x, da kuma yanayin taurari masu haɗuwa, ana ɗaukar su "mai ban mamaki", kuma wannan kamani mai ban mamaki yana nuna cewa abubuwan da suka bambanta da masu zaman kansu na iya zama sakamakon haɗuwa da taurari na neutron, kuma duka biyu na iya zama aji na kilonova transients da ba na gani ba. Saboda haka, abubuwan da suka faru a Kilonova na iya zama daban-daban kuma na kowa a sararin samaniya fiye da yadda aka fahimta a baya, a cewar masu bincike. A baya, GRB 160821B, fashewar gamma-ray da aka gano a watan Agusta 2016, yanzu an yi imanin cewa ya kasance saboda kilonova, ta hanyar kamanceceniyar bayanansa da AT2017gfo.

An kuma yi tunanin kilonova ya haifar da fashewar gamma-ray mai tsawo GRB 211211A, wanda aka gano a watan Disamba na 2021 ta Swift's Burst Alert Telescope (BAT) da Fermi Gamma-ray Burst Monitor (GBM). Wadannan binciken sun kalubalanci ka'idar da ta kasance a baya cewa GRBs masu tsawo sun fito ne kawai daga supernovae, fashewar ƙarshen rayuwa na manyan taurari. GRB 211211A ya kasance 51s;   GRB 191019A (2019)  da GRB 230307A (2023),  tare da tsawon lokaci na kusan 64s da 35s bi da bi, an kuma yi jayayya cewa suna cikin wannan aji na dogon GBRs daga Haɗuwa da tauraron neutron. 

A cikin 2023, an lura da GRB 230307A kuma an haɗa shi da tellurium da lanthanides.

 Dubi kuma 

 Hypernova
 Sabon
 Tsarin R
 Supernova
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