Quiescent H2 emission from pre-main-sequence stars in Chamaeleon I

被引:36
作者
Bary, Jeffrey S. [1 ]
Weintraub, David A. [2 ]
Shukla, Sonali J. [2 ]
Leisenring, Jarron M. [1 ]
Kastner, Joel H. [3 ]
机构
[1] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA
[2] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA
[3] Rochester Inst Technol, Carlson Ctr Imaging Sci, Rochester, NY 14623 USA
基金
美国国家科学基金会;
关键词
infrared : stars; ISM : molecules; planetary systems : protoplanetary disks; solar system : formation; stars : individual (CS Cha; HD; 97408; Sz; 33; CV Cha; GM Aur; Glass I); stars : pre-main-sequence;
D O I
10.1086/529517
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We report the discovery of quiescent emission from molecular hydrogen gas located in the circumstellar disks of six pre-main-sequence stars, including two weak-line T Tauri stars (TTSs) and one Herbig AeBe star, in the Chamaeleon I star-forming region. For two of these stars, we also place upper limits on the 2 -> 1 S(1)/1 -> 0 S(1) line ratios of similar to 0.4 and 0.5. Of the 11 pre-main-sequence sources now known to be sources of quiescent near-infrared hydrogen emission, four possess transitional disks, which suggests that detectable levels of H(2) emission and the presence of inner disk holes are correlated. These H(2) detections demonstrate that these inner holes are not completely devoid of gas, in agreement with the presence of observable accretion signatures for all four of these stars and the recent detections of [Ne II] emission from three of them. The overlap in [Ne II] and H(2) detections hints at a possible correlation between these two features and suggests a shared excitation mechanism of high-energy photons. Our models, combined with the kinematic information from the H(2) lines, locate the bulk of the emitting gas at a few tens of AU from the stars. We also find a correlation between H(2) detections and those targets which possess the largest H alpha equivalent widths, suggesting a link between accretion activity and quiescent H(2) emission. We conclude that quiescent H(2) emission from relatively hot gas within the disks of TTSs is most likely related to ongoing accretion activity, the production of UV photons and/or X-rays, and the evolutionary status of the dust grain populations in the inner disks.
引用
收藏
页码:1088 / 1098
页数:11
相关论文
共 88 条
[1]   Photoevaporation of protoplanetary discs - II. Evolutionary models and observable properties [J].
Alexander, R. D. ;
Clarke, C. J. ;
Pringle, J. E. .
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2006, 369 (01) :229-239
[2]  
Appenzeller I., 1983, Astronomy & Astrophysics Supplement Series, V53, P291
[3]   Detections of rovibrational H2 emission from the disks of T Tauri stars [J].
Bary, JS ;
Weintraub, DA ;
Kastner, JH .
ASTROPHYSICAL JOURNAL, 2003, 586 (02) :1136-1147
[4]   Detection of molecular hydrogen orbiting a "naked" T Tauri star [J].
Bary, JS ;
Weintraub, DA ;
Kastner, JH .
ASTROPHYSICAL JOURNAL, 2002, 576 (01) :L73-L76
[5]   Investigating the nature of variable class I and flat-spectrum protostars using 2-4 μm spectroscopy [J].
Beck, Tracy L. .
ASTRONOMICAL JOURNAL, 2007, 133 (04) :1673-1689
[6]   A SURVEY FOR CIRCUMSTELLAR DISKS AROUND YOUNG STELLAR OBJECTS [J].
BECKWITH, SVW ;
SARGENT, AI ;
CHINI, RS ;
GUSTEN, R .
ASTRONOMICAL JOURNAL, 1990, 99 (03) :924-945
[7]   MOLECULAR LINE EMISSION FROM CIRCUMSTELLAR DISKS [J].
BECKWITH, SVW ;
SARGENT, AI .
ASTROPHYSICAL JOURNAL, 1993, 402 (01) :280-291
[8]   Texes observations of pure rotational H2 emission from AB Aurigae [J].
Bitner, Martin A. ;
Richter, Matthew J. ;
Lacy, John H. ;
Greathouse, Thomas K. ;
Jaffe, Daniel T. ;
Blake, Geoffrey A. .
ASTROPHYSICAL JOURNAL, 2007, 661 (01) :L69-L72
[9]   FLUORESCENT EXCITATION OF INTERSTELLAR H2 [J].
BLACK, JH ;
VANDISHOECK, EF .
ASTROPHYSICAL JOURNAL, 1987, 322 (01) :412-449
[10]   Understanding the atmospheric structure of T Tauri stars - II. UV spectroscopy of RY Tau, BP Tau, RU Lupi, GW Ori and CV Cha [J].
Brooks, DH ;
Costa, VA ;
Lago, MTVT ;
Lanzafame, AC .
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2001, 327 (01) :177-190