Home

About

Advanced Search

Browse by Discipline

Scientific Societies

E-print Alerts

Add E-prints

E-print Network
FAQHELPSITE MAPCONTACT US


  Advanced Search  

 
action were performed with a contemporary stellar evolution code, which contains the most
 

Summary: action were performed with a contemporary
stellar evolution code, which contains the most
recent physics input (22). In particular, use of
this code can produce up-to-date solar models
(23) and can allow one to follow the evolution
of low-mass stars through the thermal pulses of
asymptotic giant branch (AGB) stars (24). The
nuclear network is designed preferentially to
calculate the H- and He-burning phases in low-
mass stars. Additionally, the basic reactions of
C- and O-burning are included, which may
destroy the produced C and O in massive and
intermediate-mass stars.
We performed stellar model calculations
for a typical massive, intermediate-mass, and
low-mass star with masses 20, 5, and 1.3MJ,
respectively. The stars are followed from the
onset of H-burning until the third thermal
pulse in the AGB, or until the core tempera-
ture reaches 109

  

Source: Ashoori, Raymond - Department of Physics, Massachusetts Institute of Technology (MIT)
Finkelstein, Gleb - Department of Physics, Duke University

 

Collections: Physics