H2D+ observations give an age of at least one million years for a cloud core forming Sun-like stars

被引:106
作者
Bruenken, Sandra [1 ]
Sipilae, Olli [2 ,3 ]
Chambers, Edward T. [1 ]
Harju, Jorma [2 ]
Caselli, Paola [3 ,4 ]
Asvany, Oskar [1 ]
Honingh, Cornelia E. [1 ]
Kaminski, Tomasz [5 ]
Menten, Karl M. [5 ]
Stutzki, Juergen [1 ]
Schlemmer, Stephan [1 ]
机构
[1] Univ Cologne, Inst Phys, D-50937 Cologne, Germany
[2] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland
[3] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany
[4] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England
[5] Max Planck Inst Radioastron, D-53121 Bonn, Germany
基金
欧洲研究理事会; 芬兰科学院;
关键词
HETERODYNE INSTRUMENT; CHEMISTRY; H-3(+); ORTHO-H-2; RATIO; APEX; CONSTRAINTS; DEPLETION; SOFIA; WATER;
D O I
10.1038/nature13924
中图分类号
O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];
学科分类号
07 ; 0710 ; 09 ;
摘要
The age of dense interstellar cloud cores, where stars and planets form, is a crucial parameter in star formation and difficult to measure. Some models predict rapid collapse(1,2), whereas others predict timescales of more than one million years (ref. 3). One possible approach to determining the age is through chemical changes as cloud contraction occurs, in particular through indirect measurements of the ratio of the two spin isomers (ortho/para) of molecular hydrogen, H-2, which decreases monotonically with age(4-6). This has beendone for the dense cloud core L183, for which the deuterium fractionation of diazenylium(N2H+) was used as a chemical clock to infer(7) that the core has contracted rapidly (on a timescale of less than 700,000 years). Among astronomically observable molecules, the spin isomers of the deuterated trihydrogen cation, ortho-H2D+ and para-H2D+, have the most direct chemical connections to H-2 (refs 8-12) and their abundance ratio provides a chemical clock that is sensitive to greater cloud core ages. So far this ratio has not been determined because para-H2D+ is very difficult to observe. The detection of its rotational ground-state line has only now become possible thanks to accurate measurements of its transition frequency in the laboratory(13), and recent progress in instrumentation technology(14,15). Here we report observations of ortho-and para-H2D+ emission and absorption, respectively, from the dense cloud core hosting IRAS 16293-2422 A/B, a group of nascent solar-type stars (with ages of less than 100,000 years). Using the ortho/para ratio in conjunction with chemical models, we find that the dense core has been chemically processed for at least one million years. The apparent discrepancy with the earlier N2H+ work(7) arises because that chemical clock turns off sooner than the H2D+ clock, but both results imply that star-forming dense cores have ages of about one million years, rather than 100,000 years.
引用
收藏
页码:219 / +
页数:11
相关论文
共 44 条
[1]   FIRST TIME-DEPENDENT STUDY OF H2 AND H3+ ORTHO-PARA CHEMISTRY IN THE DIFFUSE INTERSTELLAR MEDIUM: OBSERVATIONS MEET THEORETICAL PREDICTIONS [J].
Albertsson, T. ;
Indriolo, N. ;
Kreckel, H. ;
Semenov, D. ;
Crabtree, K. N. ;
Henning, Th. .
ASTROPHYSICAL JOURNAL, 2014, 787 (01)
[2]   Accurate rest frequencies of submillimeter-wave lines of H2D+ and D2H+ [J].
Amano, T ;
Hirao, T .
JOURNAL OF MOLECULAR SPECTROSCOPY, 2005, 233 (01) :7-14
[3]  
Andre P., 2000, Protostars and planets 4, P59
[4]   From filamentary clouds to prestellar cores to the stellar IMF: Initial highlights from the Herschel Gould Belt Survey [J].
Andre, Ph. ;
Men'shchikov, A. ;
Bontemps, S. ;
Koenyves, V. ;
Motte, F. ;
Schneider, N. ;
Didelon, P. ;
Minier, V. ;
Saraceno, P. ;
Ward-Thompson, D. ;
Di Francesco, J. ;
White, G. ;
Molinari, S. ;
Testi, L. ;
Abergel, A. ;
Griffin, M. ;
Henning, Th. ;
Royer, P. ;
Merin, B. ;
Vavrek, R. ;
Attard, M. ;
Arzoumanian, D. ;
Wilson, C. D. ;
Ade, P. ;
Aussel, H. ;
Baluteau, J. -P. ;
Benedettini, M. ;
Bernard, J. -Ph. ;
Blommaert, J. A. D. L. ;
Cambresy, L. ;
Cox, P. ;
Di Giorgio, A. ;
Hargrave, P. ;
Hennemann, M. ;
Huang, M. ;
Kirk, J. ;
Krause, O. ;
Launhardt, R. ;
Leeks, S. ;
Le Pennec, J. ;
Li, J. Z. ;
Martin, P. G. ;
Maury, A. ;
Olofsson, G. ;
Omont, A. ;
Peretto, N. ;
Pezzuto, S. ;
Prusti, T. ;
Roussel, H. ;
Russeil, D. .
ASTRONOMY & ASTROPHYSICS, 2010, 518
[5]   High-resolution rotational spectroscopy in a cold ion trap:: H2D+ and D2H+ [J].
Asvany, Oskar ;
Ricken, Oliver ;
Mueller, Holger S. P. ;
Wiedner, Martina C. ;
Giesen, Thomas F. ;
Schlemmer, Stephan .
PHYSICAL REVIEW LETTERS, 2008, 100 (23)
[6]   A SEARCH FOR THE ROTATIONAL TRANSITIONS OF H2D+ AT 1370 GHZ AND H3O+ AT 985 GHZ [J].
BOREIKO, RT ;
BETZ, AL .
ASTROPHYSICAL JOURNAL, 1993, 405 (01) :L39-L42
[7]   Abundant H2D+ in the pre-stellar core L1544 [J].
Caselli, P ;
van der Tak, FFS ;
Ceccarelli, C ;
Bacmann, A .
ASTRONOMY & ASTROPHYSICS, 2003, 403 (03) :L37-L41
[8]   Survey of ortho-H2D+ (11,0-11,1) in dense cloud cores [J].
Caselli, P. ;
Vastel, C. ;
Ceccarelli, C. ;
van der Tak, F. F. S. ;
Crapsi, A. ;
Bacmann, A. .
ASTRONOMY & ASTROPHYSICS, 2008, 492 (03) :703-718
[9]   Heavy water stratification in a low-mass protostar [J].
Coutens, A. ;
Vastel, C. ;
Cazaux, S. ;
Bottinelli, S. ;
Caux, E. ;
Ceccarelli, C. ;
Demyk, K. ;
Taquet, V. ;
Wakelam, V. .
ASTRONOMY & ASTROPHYSICS, 2013, 553
[10]   ON THE ORTHO:PARA RATIO OF H3+ IN DIFFUSE MOLECULAR CLOUDS [J].
Crabtree, Kyle N. ;
Indriolo, Nick ;
Kreckel, Holger ;
Tom, Brian A. ;
McCall, Benjamin J. .
ASTROPHYSICAL JOURNAL, 2011, 729 (01)