Other
Scientific paper
Dec 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004phdt........33m&link_type=abstract
Ph.D dissertation, 2004. 440 pages; United States -- Georgia: Georgia State University; 2004. Publication Number: AAT 3155325.
Other
1
Massive Stars, Microquasar, Beryllium Stars
Scientific paper
Massive O- and B-type stars evolve significantly faster than stars with cooler spectral types, so their populations include stars at many different evolutionary stages. They provide fascinating laboratories for the study of stellar evolution. In this dissertation, I investigate an unevolved massive star system as well as two particular categories of evolved stars, Be stars and microquasars.
The massive triple system HD 16429 A is largely unevolved, but I present it here as an example of the type of system that will eventually experience a disrupting supernova. I discuss the Doppler tomography technique that I used to isolate the two brightest components and my analysis of each star. The stationary component, HD 16429 Aa, is an O9.5 II star. The Ab1 component is a hotter yet less luminous O8 III-IV star, while the unseen Ab2 star is estimated to be a B0 star.
Many massive binary systems, including Be binaries, contain the final product of massive stellar evolution: a neutron star or black hole companion. Mass transfer from the less evolved star onto the compact companion generates X-ray emission, and some of these massive X-ray binaries (MXRBs) also have relativistic radio jets that closely resemble small versions of extragalactic quasars. In this dissertation I perform a spectroscopic study of the microquasar LS 5039. Based on its large eccentricity and runaway velocity, LS 5039 appears to be a recent survivor of the supernova that formed the microquasar.
Be stars are a class of B stars with circumstellar disks that cause Balmer and other line emission. The source of their disks is not well understood, but it is likely that a combination of rapid rotation and other processes contribute to their formation. There are three possible reasons for their rapid rotation: they may have been born as rapid rotators, spun up by binary mass transfer, or spun up during the MS evolution of B stars. To investigate these three formation scenarios, I am performing a photometric survey of open clusters. In this work I present the results from the first 20 clusters.
No associations
LandOfFree
The evolution of massive stars: The Be star and microquasar phenomena does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with The evolution of massive stars: The Be star and microquasar phenomena, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The evolution of massive stars: The Be star and microquasar phenomena will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1164137