G. J. Wasserburg and Y.-Z. Qian 2000 ApJ 529 L21 doi:10.1086/312455
G. J. Wasserburg1 and Y.-Z. Qian2
Show affiliationsWe present a model to explain the wide range of abundances for heavy r-process elements (mass number A > 130) at low [Fe/H]. This model requires rapid star formation and/or an initial population of supermassive stars in the earliest condensed clots of matter in order to provide a prompt or initial Fe inventory. Subsequent Fe and r-process enrichment was provided by two types of supernovae: one producing heavy r-elements with no Fe on a rather short timescale and the other producing light r-elements (A ≤ 130) with Fe on a much longer timescale.
Issue 1 (2000 January 20)
Received 1999 October 19, accepted for publication 1999 November 29
Published 1999 December 17
G. J. Wasserburg and Y.-Z. Qian 2000 ApJ 529 L21
Letizia Stanghellini et al. 2002 ApJ 575 178
Gioel Calabrese et al 2004 Class. Quantum Grav. 21 5735
Teng Hao et al 2009 Chinese Phys. Lett. 26 113201
Itzhak Bars 2001 Class. Quantum Grav. 18 3113
Subhanjoy Mohanty et al. 2005 ApJ 626 498
P Mason et al 2005 J. Phys. G: Nucl. Part. Phys. 31 S1729
K. L. Luhman et al 2005 ApJ 635 L93
Kazuya Saigo and Kohji Tomisaka 2006 ApJ 645 381
G S Bisnovatyi-Kogan and V N Rudenko 2004 Class. Quantum Grav. 21 3347