Morpho-kinematic modeling of the expanding ejecta of the extremely slow nova V1280 Scorpii

• Published in: arXiv.org
• Main Authors: Naito, Hiroyuki, Tajitsu, Akito, Valèrio A R M Ribeiro, Arai, Akira, Maehara, Hiroyuki, Kouzuma, Shinjirou, Iijima, Takashi, Okazaki, Atsuo T, Watanabe, Makoto, Takagi, Seiko, Watanabe, Fumitake, Sakon, Itsuki, Sadakane, Kozo
• Format: Paper Journal Article
• Language: English
• Published: Ithaca Cornell University Library, arXiv.org 04.05.2022
• Subjects: Dust; Ejecta; Emission; Flares; Gamma rays; Inclination angle; Light curve; Line spectra; Morphology; Novae; Physics - Astrophysics of Galaxies; Physics - High Energy Astrophysical Phenomena; Physics - Solar and Stellar Astrophysics
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.2205.02266

Morphology of nova ejecta is essential for fully understanding the physical processes involved in nova eruptions. We studied the 3D morphology of the expanding ejecta of the extremely slow nova V1280 Sco with a unique light curve. Synthetic line profile spectra were compared to the observed [O III] 4959, 5007 and [N II] 5755 emission line profiles in order to find the best-fit morphology, inclination angle, and maximum expansion velocity of the ejected shell. We derive the best fitting expansion velocity, inclination, and squeeze as \(V_{\rm exp} = 2100^{+100}_{-100}\) \,km\,s\(^{-1}\), \(i = 80^{+1}_{-3}\) deg, and \(squ = 1.0^{+0.0}_{-0.1}\) using [O III] line profiles, and \(V_{\rm exp} = 1600^{+100}_{-100}\) \,km\,s\(^{-1}\), \(i = 81^{+2}_{-4}\) deg, and \(squ = 1.0^{+0.0}_{-0.1}\) using [N II] 5755 line profile. A high inclination angle is consistent with the observational results showing multiple absorption lines originating from clumpy gases which are produced in dense and slow equatorially focused outflows. Based on additional observational features such as optical flares near the maximum light and dust formation on V1280 Sco, a model of internal shock interaction between slow ejecta and fast wind proposed for the \(\gamma\)-ray emission detected in other novae seems to be applicable to this extremely slow and peculiar nova. Increasing the sample size of novae whose morphology is studied will be helpful in addressing long-standing mysteries in novae such as the dominant energy source to power the optical light at the maximum, optical flares near the maximum, clumpiness of the ejecta, and dust formation.