[Fe II] emissions associated with the young interacting binary UY Aurigae
Abstract
We present high-resolution 1.06-1.28 μm spectra toward the interacting binary UY Aur obtained with GEMINI/NIFS and the adaptive optics system Altair. We have detected [Fe II] λ1.257 μm and He I λ1.083 μm lines from both UY Aur A (the primary source) and UY Aur B (the secondary). In [Fe II] UY Aur A drives fast and widely opening outflows with an opening angle of ∼90° along a position angle of ∼40°, while UY Aur B is associated with a redshifted knot. The blueshifted and redshifted emissions show a complicated structure between the primary and secondary. The radial velocities of the [Fe II] emission features are similar for UY Aur A and B: ∼ –100 km s{sup –1} for the blueshifted emission and ∼ +130 km s{sup –1} for the redshifted component. The He I line profile observed toward UY Aur A comprises a central emission feature with deep absorptions at both blueshifted and redshifted velocities. These absorption features may be explained by stellar wind models. The He I line profile of UY Aur B shows only an emission feature.
- Authors:
-
- Subaru Telescope, National Astronomical Observatory of Japan, 650 North A'ohoku Place, Hilo, HI 96720 (United States)
- National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan)
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States)
- Astrophysics Research Institute, Liverpool John Moores University, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF (United Kingdom)
- Institute of Astronomy and Astrophysics, Academia Sinica, P.O. Box 23-141, Taipei 10617, Taiwan (China)
- Publication Date:
- OSTI Identifier:
- 22356996
- Resource Type:
- Journal Article
- Journal Name:
- Astrophysical Journal
- Additional Journal Information:
- Journal Volume: 786; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ABSORPTION; EMISSION; IRON; MASS; OPTICS; RADIAL VELOCITY; RED SHIFT; RESOLUTION; SPECTRA; STARS; STELLAR WINDS
Citation Formats
Pyo, Tae-Soo, Hayashi, Masahiko, Beck, Tracy L., Davis, Christopher J., and Takami, Michihiro. [Fe II] emissions associated with the young interacting binary UY Aurigae. United States: N. p., 2014.
Web. doi:10.1088/0004-637X/786/1/63.
Pyo, Tae-Soo, Hayashi, Masahiko, Beck, Tracy L., Davis, Christopher J., & Takami, Michihiro. [Fe II] emissions associated with the young interacting binary UY Aurigae. United States. https://doi.org/10.1088/0004-637X/786/1/63
Pyo, Tae-Soo, Hayashi, Masahiko, Beck, Tracy L., Davis, Christopher J., and Takami, Michihiro. 2014.
"[Fe II] emissions associated with the young interacting binary UY Aurigae". United States. https://doi.org/10.1088/0004-637X/786/1/63.
@article{osti_22356996,
title = {[Fe II] emissions associated with the young interacting binary UY Aurigae},
author = {Pyo, Tae-Soo and Hayashi, Masahiko and Beck, Tracy L. and Davis, Christopher J. and Takami, Michihiro},
abstractNote = {We present high-resolution 1.06-1.28 μm spectra toward the interacting binary UY Aur obtained with GEMINI/NIFS and the adaptive optics system Altair. We have detected [Fe II] λ1.257 μm and He I λ1.083 μm lines from both UY Aur A (the primary source) and UY Aur B (the secondary). In [Fe II] UY Aur A drives fast and widely opening outflows with an opening angle of ∼90° along a position angle of ∼40°, while UY Aur B is associated with a redshifted knot. The blueshifted and redshifted emissions show a complicated structure between the primary and secondary. The radial velocities of the [Fe II] emission features are similar for UY Aur A and B: ∼ –100 km s{sup –1} for the blueshifted emission and ∼ +130 km s{sup –1} for the redshifted component. The He I line profile observed toward UY Aur A comprises a central emission feature with deep absorptions at both blueshifted and redshifted velocities. These absorption features may be explained by stellar wind models. The He I line profile of UY Aur B shows only an emission feature.},
doi = {10.1088/0004-637X/786/1/63},
url = {https://www.osti.gov/biblio/22356996},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 1,
volume = 786,
place = {United States},
year = {Thu May 01 00:00:00 EDT 2014},
month = {Thu May 01 00:00:00 EDT 2014}
}