CONSTRAINING THE MOVEMENT OF THE SPIRAL FEATURES AND THE LOCATIONS OF PLANETARY BODIES WITHIN THE AB AUR SYSTEM
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Author
Lomax, Jamie R.
Wisniewski, J.

Grady, Carol A.
McElwain, Michael W.
Hashimoto, Jun
Kudo, Tomoyuki

Kusakabe, Nobuhiko
Okamoto, Yoshiko K.
Fukagawa, Misato

Abe, Lyu
Brandner, Wolfgang
Brandt, Timothy D.

Carson, Joseph C.
Currie, T.

Egner, Sebastian
Feldt, Markus
Goto, Miwa
Guyon, Olivier
Hayano, Y.

Hayashi, Masahiko

Hayashi, Saeko S.
Henning, Thomas

Hodapp, K. W.

Inoue, Akio
Ishii, Miki
Iye, Masanori
Janson, M.

Kandori, Ryo
Knapp, G. R.

Kuzuhara, Masayuki
Kwon, J.

Matsuo, Taro
Mayama, Satoshi
Miyama, Shoken

Momose, Munetake

Morino, Jun-Ichi
Moro-Martin, A.

Nishimura, Tetsuo
Pyo, T.-S.

Schneider, Glenn

Serabyn, Eugene
Sitko, Michael

Suenaga, Takuya
Suto, Hiroshi
Suzuki, Ryuji
Takahashi, Yasuhiro H.
Takami, M.

Takato, Naruhisa
Terada, H.

Thalmann, C.

Tomono, Daigo
Turner, Edwin L.
Watanabe, M.

Yamada, Toru
Takami, Hideki
Usuda, T.

Tamura, Motohide

Affiliation
Univ Arizona, Steward ObservIssue Date
2016-08-22Keywords
planet-disk interactionsplanetary systems
protoplanetary disks
radiative transfer
stars: individual (AB Aur)
stars: pre-main sequence
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IOP PUBLISHING LTDCitation
CONSTRAINING THE MOVEMENT OF THE SPIRAL FEATURES AND THE LOCATIONS OF PLANETARY BODIES WITHIN THE AB AUR SYSTEM 2016, 828 (1):2 The Astrophysical JournalJournal
The Astrophysical JournalRights
© 2016. The American Astronomical Society. All rights reserved.Collection Information
This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.Abstract
We present a new analysis of multi-epoch, H-band, scattered light images of the AB Aur system. We use a Monte Carlo radiative transfer code to simultaneously model the system's spectral energy distribution (SED) and H-band polarized intensity (PI) imagery. We find that a disk-dominated model, as opposed to one that is envelope-dominated, can plausibly reproduce AB Aur's SED and near-IR imagery. This is consistent with previous modeling attempts presented in the literature and supports the idea that at least a subset of AB Aur's spirals originate within the disk. In light of this, we also analyzed the movement of spiral structures in multi-epoch H-band total light and PI imagery of the disk. We detect no significant rotation or change in spatial location of the spiral structures in these data, which span a 5.8-year baseline. If such structures are caused by disk-planet interactions, the lack of observed rotation constrains the location of the orbit of planetary perturbers to be >47 au.ISSN
1538-4357Version
Final published versionSponsors
NASA Origins of Solar System program [NNX13AK17G, RTOP 12-OSS12-0045, NNG13PB64P]; MEXT Japan; Mitsubishi Foundation; [NSF-AST 1009203]; [1008440]; [1009314]Additional Links
http://stacks.iop.org/0004-637X/828/i=1/a=2?key=crossref.3d2c6f18ef5537b557b848ddf53457b6ae974a485f413a2113503eed53cd6c53
10.3847/0004-637X/828/1/2