V1647 Orionis (IRAS 05436-0007) in outburst: The first three months

Frederick M. Walter; Guy S. Stringfellow; William H. Sherry; Angeliki Field-Pollatou

doi:10.1086/423703

V1647 Orionis (IRAS 05436-0007) in outburst: The first three months

Frederick M. Walter
, Guy S. Stringfellow
, William H. Sherry
, Angeliki Field-Pollatou

Physics and Astronomy

University of Colorado Boulder
Stony Brook University

Research output: Contribution to journal › Article › peer-review

32 Scopus citations

Abstract

We report on photometric (BVRIJHK) and low-dispersion spectroscopic observations of V1647 Orionis, the star that drives McNeil's Nebula, between 2004 February 10 and May 7. The star is photometrically variable atop a general decline in brightness of about 0.3-0.4 mag during these 87 days. The spectra are featureless, aside from Hα and the Ca II infrared triplet in emission and a Na II D absorption feature. The Ca II triplet line ratios are typical of young stellar objects. The Ha equivalent width may be modulated on a period of about 60 days. The postoutburst extinction appears to be less than 7 mag. The data are suggestive of an FU Orionis-like event, but further monitoring will be needed to definitively characterize the outburst.

Original language	English
Pages (from-to)	1872-1879
Number of pages	8
Journal	Astronomical Journal
Volume	128
Issue number	4
DOIs	https://doi.org/10.1086/423703
State	Published - Oct 2004

Keywords

Stars: individual (V1647 Orionis, IRAS 05436-0007)
Stars: pre-main-sequence

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10.1086/423703

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title = "V1647 Orionis (IRAS 05436-0007) in outburst: The first three months",

abstract = "We report on photometric (BVRIJHK) and low-dispersion spectroscopic observations of V1647 Orionis, the star that drives McNeil's Nebula, between 2004 February 10 and May 7. The star is photometrically variable atop a general decline in brightness of about 0.3-0.4 mag during these 87 days. The spectra are featureless, aside from Hα and the Ca II infrared triplet in emission and a Na II D absorption feature. The Ca II triplet line ratios are typical of young stellar objects. The Ha equivalent width may be modulated on a period of about 60 days. The postoutburst extinction appears to be less than 7 mag. The data are suggestive of an FU Orionis-like event, but further monitoring will be needed to definitively characterize the outburst.",

keywords = "Stars: individual (V1647 Orionis, IRAS 05436-0007), Stars: pre-main-sequence",

author = "Walter, \{Frederick M.\} and Stringfellow, \{Guy S.\} and Sherry, \{William H.\} and Angeliki Field-Pollatou",

year = "2004",

month = oct,

doi = "10.1086/423703",

language = "English",

volume = "128",

pages = "1872--1879",

journal = "Astronomical Journal",

issn = "0004-6256",

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TY - JOUR

T1 - V1647 Orionis (IRAS 05436-0007) in outburst

T2 - The first three months

AU - Walter, Frederick M.

AU - Stringfellow, Guy S.

AU - Sherry, William H.

AU - Field-Pollatou, Angeliki

PY - 2004/10

Y1 - 2004/10

N2 - We report on photometric (BVRIJHK) and low-dispersion spectroscopic observations of V1647 Orionis, the star that drives McNeil's Nebula, between 2004 February 10 and May 7. The star is photometrically variable atop a general decline in brightness of about 0.3-0.4 mag during these 87 days. The spectra are featureless, aside from Hα and the Ca II infrared triplet in emission and a Na II D absorption feature. The Ca II triplet line ratios are typical of young stellar objects. The Ha equivalent width may be modulated on a period of about 60 days. The postoutburst extinction appears to be less than 7 mag. The data are suggestive of an FU Orionis-like event, but further monitoring will be needed to definitively characterize the outburst.

AB - We report on photometric (BVRIJHK) and low-dispersion spectroscopic observations of V1647 Orionis, the star that drives McNeil's Nebula, between 2004 February 10 and May 7. The star is photometrically variable atop a general decline in brightness of about 0.3-0.4 mag during these 87 days. The spectra are featureless, aside from Hα and the Ca II infrared triplet in emission and a Na II D absorption feature. The Ca II triplet line ratios are typical of young stellar objects. The Ha equivalent width may be modulated on a period of about 60 days. The postoutburst extinction appears to be less than 7 mag. The data are suggestive of an FU Orionis-like event, but further monitoring will be needed to definitively characterize the outburst.

KW - Stars: individual (V1647 Orionis, IRAS 05436-0007)

KW - Stars: pre-main-sequence

UR - https://www.scopus.com/pages/publications/9344233272

U2 - 10.1086/423703

DO - 10.1086/423703

M3 - Article

AN - SCOPUS:9344233272

SN - 0004-6256

VL - 128

SP - 1872

EP - 1879

JO - Astronomical Journal

JF - Astronomical Journal

IS - 4

ER -

V1647 Orionis (IRAS 05436-0007) in outburst: The first three months

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Keywords

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