Common envelope jets supernova
Common envelope jets supernova (CEJSN) is a type of supernova, where the explosion is caused by the merger of a giant or supergiant star with a compact star such as a neutron star or a black hole. As the compact star plunges into the envelope of the giant/supergiant, it begins to accrete matter from the envelope and launches jets that can disrupt the envelope. Often, the compact star eventually merges with the core of the giant/supergiant; other times the infall stops before core merger.
This kind of supernova has been invoked to explain certain kinds of supernova-like phenomena, including iPTF14hls.
History and process
In order to explain the unusual
In their model, iPTF14hls was a binary star consisting of a giant star and a neutron star. The latter plunged into the envelope of the former and began to accrete material, emitting neutrinos as it did so but without substantially deforming the giant.[3] Eventually, it would have reached the core of the giant and accreted mass at a sufficient rate to produce jets. These jets emanate from the polar areas of the neutron star and can effectively eject matter in these directions, but do not effectively act on material accreting along the neutron star's equatorial plane, which thus continues to reach the neutron star.[4] The jets impact the envelope, inflating it in the form of large bubbles ("cocoons"[5]) that remove material from the envelope[6] at speeds approaching a tenth of the speed of light.[7] This causes the envelope of the giant star to be ejected over a timespan of a few hundred days, before the core itself is consumed in about a day,[8] producing gravitational waves.[9] The exiting jets can interact with pre-existent gas clouds around the giant, which creates the luminosity of the supernova[10] and which can last for timespans reaching years.[11]
Depending on the original architecture of the stellar system, many variations on this general process are possible,
There are several processes that can cause the neutron star to penetrate the giant. Giant stars grow in size just at the end of their evolution, and can envelop a companion star in the process. When a star goes supernova and produces a neutron star, the neutron star receives a "kick" that causes it to penetrate the other star. Finally, interactions between the neutron star-giant binary with a third star, typically the third member star of the group, can cause the neutron star orbit to contract until it interacts with the envelope of the giant.[17]
Concomitant processes
Already before the actual penetration, tidal acceleration of the giant's envelope by the neutron star causes it to expand, possibly clearing the polar regions of the giant of matter before the merger begins. This lets the jets exit the star from the poles before the neutron star merges with the core; otherwise they are only visible at the beginning of the envelope interaction or when the actual core interacts with the neutron star.[18] The energy that the jets inject into the envelope can cause it to expand so that even when the orbit takes the neutron star out of the envelope, accretion and jet launching continue. These jets are weaker than the ones launched inside the original envelope, but are more efficient at creating radiation as they interact with already-emplaced gas.[19]
A key requirement for the occurrence of a common envelope jets supernova is that the neutron star can form an
The conditions during a CEJSN may allow the r-process of nucleosynthesis to take place[16] in the jets,[21] in particular when a binary neutron star is involved,[12] since unlike the core of a conventional supernova the CEJSN is not an effective neutrino source.[22] Unlike regular neutron star mergers, the CEJSN is not delayed by the time it takes for the neutron star binary to shrink from gravitational wave emission and thus CEJSN can contribute r-process elements early in the history of the universe.[23] The r-process element enrichment of the galaxy Reticulum II may be explained through a CEJSN, which efficiently distributed r-process elements across the galaxy.[24]
Examples
Apart from iPTF14hls, other events such as the supernovae SN1979c, SN1998e,[5] SN2019zrk,[25] SN 2020faa and the radio transient VT J121001+495647 have been proposed to be CEJSNs. The gamma-ray burst GRB 101225A could have formed through a common envelope jets supernova-like interaction with a helium star.[16] A CEJSN where the core of the companion star was disrupted may have given rise to the enigmatic supernova remnant W49B.[26] Fast blue optical transients might constitute CEJSNs as well.[7]
Impostors
This process does not always result in the immediate destruction of the giant; if the giant star survives, a
References
- ^ Soker & Gilkis 2018, pp. 1198–1199.
- ^ Akashi & Soker 2021, p. 9.
- ^ Soker & Gilkis 2018, p. 1199.
- ^ Soker & Gilkis 2018, p. 1200.
- ^ a b Ragoler et al. 2022, p. 2.
- ^ a b Gilkis, Soker & Kashi 2019, p. 4236.
- ^ a b c Soker 2022, p. 2.
- ^ Soker & Gilkis 2018, p. 1201.
- ^ Soker 2019, p. 6.
- ^ Soker 2022, p. 5.
- ^ Soker 2021, p. 1.
- ^ a b Akashi & Soker 2021, p. 1.
- ^ Soker 2021, p. 7.
- ^ Soker 2021, p. 8.
- ^ Grichener & Soker 2023, p. 6042.
- ^ a b c Soker 2022, p. 1.
- ^ a b c Gilkis, Soker & Kashi 2019, p. 4234.
- ^ Soker 2022, p. 4.
- ^ Ragoler et al. 2022, p. 6.
- ^ a b Gilkis, Soker & Kashi 2019, p. 4235.
- ^ Grichener & Soker 2019, p. 11.
- ^ Grichener & Soker 2019, p. 1.
- ^ Soker 2021, p. 9.
- ^ Grichener & Soker 2022.
- ^ Soker 2022b, p. 8.
- ^ Grichener & Soker 2023, p. 6044.
- ^ Gilkis, Soker & Kashi 2019, p. 4239.
- ^ a b Soker 2022, p. 11.
- ^ Gilkis, Soker & Kashi 2019, p. 4241.
- ^ Soker 2022, p. 3.
Sources
- Akashi, Muhammad; Soker, Noam (December 2021). "Simulating the Outcome of a Binary Neutron Star Merger in a Common Envelope Jets Supernova". The Astrophysical Journal. 923 (1): 55. ISSN 0004-637X.
- Gilkis, Avishai; Soker, Noam; Kashi, Amit (21 January 2019). "Common envelope jets supernova (CEJSN) impostors resulting from a neutron star companion". Monthly Notices of the Royal Astronomical Society. 482 (3): 4233–4242. .
- Grichener, Aldana; Soker, Noam (June 2019). "The Common Envelope Jet Supernova (CEJSN) r-process Scenario". The Astrophysical Journal. 878 (1): 24. ISSN 0004-637X.
- Grichener, Aldana; Soker, Noam (December 2022). "The Implications of Ultra-Faint Dwarf Galaxy Reticulum II on the Common Envelope Jets Supernova r-process Scenario". Research Notes of the AAS. 6 (12): 263. ISSN 2515-5172.
- Grichener, Aldana; Soker, Noam (22 June 2023). "Common envelope jets supernova with thermonuclear outburst progenitor for the enigmatic supernova remnant W49B". Monthly Notices of the Royal Astronomical Society. 523 (4): 6041–6047. .
- Ragoler, Nitzan; Bear, Ealeal; Schreier, Ron; Hillel, Shlomi; Soker, Noam (18 August 2022). "The response of a red supergiant to a common envelope jets supernova (CEJSN) impostor event". Monthly Notices of the Royal Astronomical Society. 515 (4): 5473–5478. doi:10.1093/mnras/stac2148 – via arXiv.
- Soker, Noam; Gilkis, Avishai (2018). "Explaining iPTF14hls as a common-envelope jets supernova". Monthly Notices of the Royal Astronomical Society. 475 (1): 1198–1202. .
- Soker, Noam (17 May 2019). "The class of supernova progenitors that result from fatal common envelope evolution". Science China Physics, Mechanics & Astronomy. 62 (11): 119501. S2CID 255203912.
- Soker, Noam (20 July 2021). "Binary neutron star merger in common envelope jets supernovae". Monthly Notices of the Royal Astronomical Society. 506 (2): 2445–2452. doi:10.1093/mnras/stab1860 – via arXiv.
- Soker, Noam (April 2022). "A Common Envelope Jets Supernova (CEJSN) Impostor Scenario for Fast Blue Optical Transients". Research in Astronomy and Astrophysics. 22 (5): 055010. S2CID 246036031.
- Soker, Noam (24 September 2022b). "Pre-explosion, explosion, and post-explosion jets in supernova SN 2019zrk". Monthly Notices of the Royal Astronomical Society. 516 (4): 4942–4948. doi:10.1093/mnras/stac2592 – via arXiv.