V1647 ORIONIS: OPTICAL PHOTOMETRIC AND SPECTROSCOPIC MONITORING THROUGH THE 2003-2006 OUTBURST

Journal Article · Thu Oct 15 04:00:00 EDT 2009 · Astronomical Journal (New York, N.Y. Online)

DOI:https://doi.org/10.1088/0004-6256/138/4/1137; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA)· OSTI ID:21301587

Aspin, Colin; Reipurth, Bo ^[1]

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1. Institute for Astronomy, University of Hawaii, 640 N. A'ohoku Place, Hilo, HI 96720 (United States)

We present results from an optical imaging and spectroscopic monitoring campaign on the young, low-mass eruptive variable star V1647 Orionis. The star and associated nebulosity (McNeil's Nebula) were observed over the period 2004 February to 2006 February with observations commencing a few months after the original outburst event occurred. Using the Gemini North telescope, we obtained multiband optical imaging photometry and medium-resolution long-slit spectroscopy of V1647 Ori on an approximately monthly interval. During this period, V1647 Ori remained at, or close to, peak brightness and then faded by 5 mag to close to its pre-outburst brightness. This implies an outburst timescale of around 27 months. Spectral features seen in both emission and absorption varied considerably during the monitoring period. For example, the H{alpha} line changed significantly in both intensity and profile. We present and discuss the observed photometric and spectroscopic changes and consider how this eruptive event relates to the early formative stages of low-mass stars.

• OSTI ID: 21301587
• Journal Information: Astronomical Journal (New York, N.Y. Online), Journal Name: Astronomical Journal (New York, N.Y. Online) Journal Issue: 4 Vol. 138; ISSN 1538-3881
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
99 GENERAL AND MISCELLANEOUS
ABSORPTION
ACCRETION DISKS
BRIGHTNESS
ERUPTIVE VARIABLE STARS
MASS
NEBULAE
PHOTOMETRY
SPECTROSCOPY
STAR ACCRETION
TELESCOPES