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Detection of a Proto-planetary Clump in the Habitable Zone of GM Cephei

Published online by Cambridge University Press:  29 April 2014

W. P. Chen
Affiliation:
Graduate Institute of Astronomy, National Central University, 300 Jhongda Road, Jhongli 32001, Taiwan email: [email protected]
S. C.-L. Hu
Affiliation:
Graduate Institute of Astronomy, National Central University, 300 Jhongda Road, Jhongli 32001, Taiwan email: [email protected] Taipei Astronomical Museum, 363 Jihe Rd., Shilin, Taipei 11160, Taiwan
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Abstract

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GM Cephei is an active T Tauri star in the young open cluster Trumpler 37, showing abrupt UX Orionis type of photometric variability. Its light curves exhibit frequent, sporadic brightening events, each of <0.5 mag and lasting for days, which must have been originated from unsteady circumstellar accretion. In addition, the star undergoes a brightness drop up to ~1 mag lasting for about a month, during which the star became bluer when fainter. Moreover, the brightness drops seem to have a recurrence timescale of about 300 days. It is proposed that the brightness drop arises from obscuration of the central star by an orbiting dust concentration, exemplifying disk inhomogeneity in transition between grain coagulation and planetesimal formation in a young circumstellar disk. GM Cep was found to show a few percent polarization in the optical wavelengths, and an enhanced level of polarization during the occultation phase.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2014 

References

Bouvier, J., et al. 2003, A&A, 409, 169Google Scholar
Briceño, C., et al. 2007, ApJ, 661, 1119CrossRefGoogle Scholar
Chen, W. P., et al. 2012, ApJ, 751, 118Google Scholar
Contreras, M. E., et al. 2002, AJ, 124, 1585CrossRefGoogle Scholar
Goldreich, P. & Ward, W. 1973, ApJ, 183, 1051Google Scholar
Grinin, V. P., Rostopchina, A. N., & Shakhovskoi, D. N. 1998, Ast. Lett., 24, 802Google Scholar
Herbst, W., Herbst, D. K., Grossman, E. J., & Weinstein, D. 1994, AJ, 108, 1906Google Scholar
Herbst, W. & Shevchenko, V. S. 1999, AJ, 118, 1043Google Scholar
Hillenbrand, L. A. 2008, Phys. Scr., 130, 4024Google Scholar
Hillenbrand, L. A., et al. 2013, AJ 145 article id. 59Google Scholar
Johansen, Anders, et al. 2007, Nature, 448, 1022Google Scholar
Mamajek, E. E.et al. 2004, ApJ, 612, 496Google Scholar
Marschall, L. A., Karshner, G. B., & Comins, N. F. 1990, AJ, 99, 1536Google Scholar
Neuäuser, , et al. 2011, AN, 332, 527Google Scholar
Patel, N., et al. 1995, ApJ, 447, 721Google Scholar
Safronov, V. S. 1972, in Evolution of the protoplanetary cloud and formation of the earth and planets, Jerusalem: Keter Publishing HouseGoogle Scholar
Semkov, E. H. & Peneva, S. P. 2012, Ap&SS, 338, 95Google Scholar
Sicilia-Aguilar, A., et al. 2005, AJ, 130, 188CrossRefGoogle Scholar
Sicilia-Aguilar, A., et al. 2008, ApJ, 673, 382Google Scholar
Weidenschilling, S. 2000, Sp. Sci. Rev., 92, 295Google Scholar
Xiao, L., Kroll, P., & Henden, A. 2010, A, 139, 1527Google Scholar