2019/10/17 by Mizuho Uchiyama, Takuya Yamashita, Koichiro Sugiyama +10 · 19 citations
Physics and Astronomy · #Accretion (finance) #Accretion disc #Astrophysical Phenomena and Observations #Astrophysics and Star Formation Studies #Event (particle physics) #Flux (metallurgy) #Gamma-ray bursts and supernovae #Infrared #Light curve #Maser #Young stellar object #astro-ph.GA #astro-ph.SR
paper · pdf · doi:10.1093/pasj/psz122
published in Publications of the Astronomical Society of Japan 72(1) (Oxford University Press) · 8 pages, 4 figures, 2 tables, accepted to PASJ
arxiv created 2019/10/17 · openalex publication_date 2019/10/22 · openalex created_date 2019/10/25 · arxiv updated 2020/01/08 · openalex updated_date 2026/08/05
Abstract We followed up the massive young stellar object S255-NIRS3 (= S255-IRS1b) during its recent accretion outburst event in the K\rm s band with Kanata/HONIR for four years after its burst and obtained a long-term light curve. This is the most complete near-infrared light curve of the S255-NIRS3 burst event that has ever been presented. The light curve showed a steep increase reaching a peak flux that was 3.4 mag brighter than the quiescent phase and then a relatively moderate year-scale fading until the last observation, similar to that of the accretion burst events such as EXors found in lower-mass young stellar objects. The behavior of the K\rm s-band light curve is similar to that observed in 6.7 GHz class II methanol maser emission, with a sudden increase followed by moderate year-scale fading. However, the maser emission peaks appear 30–50 d earlier than that of the K\rm s band emission. The similarities confirmed that the origins of the maser emission and the K\rm s-band continuum emission are common, as previously shown from other infrared and radio observations by Stecklum et al. (2016, Astronomer’s Telegram, 8732), Caratti o Garatti et al. (2017b, Nature Phys., 13, 276), and Moscadelli et al. (2017, A&A, 600, L8). However, the differences in energy transfer paths, such as the exciting/emitting/scattering structures, may cause the delay in the flux-peak dates.