After the 2020 event, the orbital period can be reconciled to 2022.9 d. for all the datasets including the 1981 one, so the period change around 1998 is not supported.
Possibly the most massive heartbeat binary according to 2018arXiv180105445R. A pulsation period of 58.8 d. was found. On January 2018, eta Carinae is around V= 4.3 with small amplitude fluctuations (~0.1 mag.). The elements given in the table are for the recent visual minima accompanying the X-ray minima. Historical data reveal several period changes coincident with mass ejection events. Before the 1844 eruption P= 1922 d. Second eruption in 1887. Third smaller eruption in 1941 (2011MNRAS.415.2009S). Fourth eruption in 1998. Period between 1981-1998 was 2020 d. After 1998 P= 2024 d. according to visual and V data from AAVSO, OALP and Otero.
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GCVS Team
In the emission nebula NGC 3372 in the region of the cluster Tr 16. A very massive young star surrounded by an expanding gas and dust shell with the diameter 2" at 2mu and 6.5" at 12.2mu. Maximum brightness was observed in 1843. Since 1880 varies in the range 5.9 - 7.9 V. In the interval JD2434000 - 41000 Max = 2434037 + 1110d*E. There are emission lines of H, HeI, FeII, [FeII], etc. in the spectrum. Description of the spectrum [N.R.Walborn, M.H.Liller, ApJ 211, 181, 1977., R.Viotti, Mem SAIt 39, N1, 105, 1968.]. Soft X-ray source of variable intensity.
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