SOLAR-C Project Team
Profile Information
- Affiliation
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency
- Degree
- 博士（理学）(東京大学大学院)
- Researcher number
- 70795624
- ORCID ID
https://orcid.org/0000-0002-6681-7318- J-GLOBAL ID
- 201801011232252049
- researchmap Member ID
- B000318417
赤外線天文学、観測装置開発、星形成（大質量星）、時間天文学
Research Areas
1Major Research History
4-
Apr, 2020 - Aug, 2021
Education
3-
Apr, 2012 - May, 2015
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Apr, 2010 - Mar, 2012
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Apr, 2006 - Mar, 2010
Major Papers
39-
Publications of the Astronomical Society of Japan, Feb 1, 2020 Peer-reviewed<jats:title>Abstract</jats:title> <jats:p>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.</jats:p>
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The Astrophysical Journal, 883(1) 6-6, Sep 17, 2019 Peer-reviewed
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ADVANCES IN OPTICAL AND MECHANICAL TECHNOLOGIES FOR TELESCOPES AND INSTRUMENTATION, 9151(915143) 9, 2014
Misc.
29-
Space Telescopes and Instrumentation 2020: Optical, Infrared, and Millimeter Wave, Dec 13, 2020
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(17) 249-251, Mar 9, 2018SPICA Science Conference from Exoplanets to Distant Galaxies: SPICA's New Window on the Cool Universe (June 18-21, 2013. Ito Hall, the University of Tokyo), Bunkyou-ku, Tokyo, JapanWe present a result of high-resolution 30 μm imaging observations of the Homunculus Nebula of Eta Carinae (η Car). The Homunculus Nebula is known to contain a large amount of cool dust (approximately 100 K) at polar lobes and a equatorial torus. While the distribution of the cool dust shows the past dust formation events on Car such as giant eruptions and binary interactions, no spatially resolved images at long mid-infrared wavelengths (30-50 μm) have been obtained. We observed Car with a mid-infrared camera MAX38 on the University of Tokyo Atacama 1.0-m telescope, and successfully obtained spatially resolved images of the Homunculus Nebula at 18.7, 31.7 and 37.3 μm. The observations revealed the structure of the massive equatorial torus which contains the dust of 0.09 solar mass. This amount is equal to approximately 80% of the total dust mass 0.12 solar mass in the Homunculus Nebula. It is also found that the dust of 0.012 solar mass exists inside the polar lobes. Assuming that the dust was constantly formed after the giant eruption occurred in 1843, the dust formation rate is estimated as 7 × 10(exp -5)solar mass yr(exp -1). This indicates that the binary interaction plays a significant role in the dust formation on Car.Number of authors: 29Physical characteristics: Original contains color illustrations
