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Diagnosing the Clumpy Protoplanetary Disk of the UXor Type Young Star GM Cephei
Huang, P. C.1; Chen, W. P.1,2; Mugrauer, M.3,4; Bischoff, R.3,4; Budaj, J.5; Burkhonov, O.6; Ehgamberdiev, S.6; Errmann, R.7,8; Garai, Z.5; Hsiao, H. Y.1; Hu, C. L.9; Janulis, R.10; Jensen, E. L. N.11; Kiyota, S.12; Kuramoto, K.13; Lin, C. S.1; Lin, H. C.1; Liu, J. Z.14; Lux, O.3,4; Naito, H.15; Neuhaeuser, R.3,4; Ohlert, J.16,17; Pakstiene, E.18; Pribulla, T.5; Qvam, J. K. T.19; Raetz, St.20,21; Sato, S.22; Schwartz, M.23; Semkov, E.24,25; Takagi, S.13; Wagner, D.3,4; Watanabe, M.26; Zhang, Yu14
Contribution Rank13
AbstractUX Orionis stars (UXors) are Herbig Ae/Be or T Tauri stars exhibiting sporadic occultation of stellar light by circumstellar dust. GM Cephei is such a UXor in the young (similar to 4 Myr) open cluster Trumpler 37, showing prominent infrared excess, emission-line spectra, and flare activity. Our photometric monitoring (2008-2018) detects (1) an similar to 3.43 day period, likely arising from rotational modulation by surface starspots, (2) sporadic brightening on timescales of days due to accretion, (3) irregular minor flux drops due to circumstellar dust extinction, and (4) major flux drops, each lasting for a couple of months with a recurrence time, though not exactly periodic, of about two years. The star experiences normal reddening by large grains, i.e., redder when dimmer, but exhibits an unusual "blueing" phenomenon in that the star turns blue near brightness minima. The maximum extinction during relatively short (lasting <= 50 days) events, is proportional to the duration, a consequence of varying clump sizes. For longer events, the extinction is independent of duration, suggestive of a transverse string distribution of clumps. Polarization monitoring indicates an optical polarization varying similar to 3%-8%, with the level anticorrelated with the slow brightness change. Temporal variation of the unpolarized and polarized light sets constraints on the size and orbital distance of the circumstellar clumps in the interplay with the young star and scattering envelope. These transiting clumps are edge-on manifestations of the ring- or spiral-like structures found recently in young stars with imaging in infrared of scattered light, or in submillimeter of thermalized dust emission.
Keywordcircumstellar matter occultations protoplanetary disks stars: individual (GM Cephei) stars: pre-main sequence stars: variables: T Tauri, Herbig Ae/Be
Indexed BySCI
Funding Projectprogram of the light in China's Western Region (LCWR)[2015-XBQN-A-02] ; National Natural Science Foundation of China[11661161016] ; Thuringian State (Thuringer Ministerium fur Bildung, Wissenschaft und Kultur)[B 515-07010] ; [MOST 106-2112-M-008-005-MY3] ; [MOST 105-2119-M-008-028-MY3] ; [VEGA 2/0031/18] ; [APVV 15-0458]
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000457281200016
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Cited Times:1[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Corresponding AuthorHuang, P. C.
Affiliation1.Natl Cent Univ, Grad Inst Astron, 300 Zhongda Rd, Taoyuan 32001, Taiwan
2.Natl Cent Univ, Dept Phys, 300 Zhongda Rd, Taoyuan 32001, Taiwan
3.Univ Sternwarte, Astrophys Inst, Schillergasschen 2-3, D-07745 Jena, Germany
4.Univ Sternwarte, FSU Jena, Schillergasschen 2-3, D-07745 Jena, Germany
5.Slovak Acad Sci, Astron Inst, Tatranska Lomnica 05960, Slovakia
6.Uzbek Acad Sci, Ulugh Beg Astron Inst, 33 Astronomicheskaya str, Tashkent 100052, Uzbekistan
7.Univ Hertfordshire, CAR, Hatfield AL10 9AB, Herts, England
8.Friedrich Schiller Univ Jena, Abbe Ctr Photon, Max Wien Pl 1, D-07743 Jena, Germany
9.Taipei Astron Museum, 363 Jihe Rd, Taipei 11160, Taiwan
10.Vilnius Univ, Inst Theoret Phys & Astrophys, Sauletekio Av 3, LT-10257 Vilnius, Lithuania
11.Swarthmore Coll, Dept Phys & Astron, 500 Coll Ave, Swarthmore, PA 19081 USA
12.VSOLJ, 7-Kitahatsutomi, Kamagaya, Chiba 2730126, Japan
13.Hokkaido Univ, Dept Cosmosci, Kita Ku, Kita 10,Nishi 8, Sapporo, Hokkaido 0600810, Japan
14.Chinese Acad Sci, Xinjiang Observ, Natl Astron Observ, 150 Sci 1-St, Urumqi 830011, Xinjiang, Peoples R China
15.Nayoro Observ, 157-1 Nisshin, Nayoro, Hokkaido 0960066, Japan
16.Univ Appl Sci, Wilhelm Leuschner Str 13, D-61169 Friedberg, Germany
17.Astron Stiftung Trebur, Michael Adrian Observ, Fichtenstr 7, D-65768 Trebur, Germany
18.Vilnius Univ, Inst Theoret Phys & Astron, Sauletekio Av 3, LT-10257 Vilnius, Lithuania
19.Univ Oslo, Dept Phys, POB 1048, NO-0316 Oslo, Norway
20.Univ Freiburg, Freiburg Inst Adv Studies FRIAS, Albertstr 19, D-79104 Freiburg, Germany
21.Univ Tubingen, IAAT, Sand 1, D-72076 Tubingen, Germany
22.Nagoya Univ, Dept Astrophys, Nagoya, Aichi 4648602, Japan
23.Tenagra Observ, 221 Calle Coco, Rio Rico, AZ 85648 USA
24.Bulgarian Acad Sci, Inst Astron, 72 Tsarigradsko Shosse Blvd, Sofia 1784, Bulgaria
25.Bulgarian Acad Sci, Natl Astron Observ, 72 Tsarigradsko Shosse Blvd, Sofia 1784, Bulgaria
26.Okayama Univ Sci, Dept Appl Phys, Kita Ku, 1-1 Ridai Cho, Okayama, Okayama 700005, Japan
Recommended Citation
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Huang, P. C.,Chen, W. P.,Mugrauer, M.,et al. Diagnosing the Clumpy Protoplanetary Disk of the UXor Type Young Star GM Cephei[J]. ASTROPHYSICAL JOURNAL,2019,871(2):183.
APA Huang, P. C..,Chen, W. P..,Mugrauer, M..,Bischoff, R..,Budaj, J..,...&Zhang, Yu.(2019).Diagnosing the Clumpy Protoplanetary Disk of the UXor Type Young Star GM Cephei.ASTROPHYSICAL JOURNAL,871(2),183.
MLA Huang, P. C.,et al."Diagnosing the Clumpy Protoplanetary Disk of the UXor Type Young Star GM Cephei".ASTROPHYSICAL JOURNAL 871.2(2019):183.
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