Close binary interactions may play a critical role in the formation of the rapidly rotating Be stars. Mass transfer can result in a mass gainer star spun up by the accretion of mass and angular momentum, while the mass donor is stripped of its envelope to form a hot and faint helium star. Far-UV spectroscopy has led to the detection of about 20 such binary Be+sdO systems. Here we report on a 3 yr program of high-quality spectroscopy designed to determine the orbital periods and physical properties of five Be binary systems. These binaries are long orbital period systems with
- Home
- Search Results
- Page 1 of 1
Search for: All records
-
Total Resources2
- Resource Type
-
00020
- Availability
-
20
- Author / Contributor
- Filter by Author / Creator
-
-
Gies, Douglas R. (2)
-
Peters, Geraldine J. (2)
-
Butterley, Tim (1)
-
Dhillon, Vik S. (1)
-
Guo, Zhao (1)
-
Han, Zhanwen (1)
-
Lester, Kathryn V. (1)
-
Littlefair, Stuart P. (1)
-
Matson, Rachel A. (1)
-
Maxted, Pierre F. (1)
-
Wang 王璐, Luqian 茜. (1)
-
Wang, Luqian (1)
-
Wilson, Richard W. (1)
-
#Tyler Phillips, Kenneth E. (0)
-
#Willis, Ciara (0)
-
& Abreu-Ramos, E. D. (0)
-
& Abramson, C. I. (0)
-
& Abreu-Ramos, E. D. (0)
-
& Adams, S.G. (0)
-
& Ahmed, K. (0)
-
- Filter by Editor
-
-
& Spizer, S. M. (0)
-
& . Spizer, S. (0)
-
& Ahn, J. (0)
-
& Bateiha, S. (0)
-
& Bosch, N. (0)
-
& Brennan K. (0)
-
& Brennan, K. (0)
-
& Chen, B. (0)
-
& Chen, Bodong (0)
-
& Drown, S. (0)
-
& Ferretti, F. (0)
-
& Higgins, A. (0)
-
& J. Peters (0)
-
& Kali, Y. (0)
-
& Ruiz-Arias, P.M. (0)
-
& S. Spitzer (0)
-
& Spitzer, S. (0)
-
& Spitzer, S.M. (0)
-
(submitted - in Review for IEEE ICASSP-2024) (0)
-
- (0)
-
-
Have feedback or suggestions for a way to improve these results?
!
Note: When clicking on a Digital Object Identifier (DOI) number, you will be taken to an external site maintained by the publisher.
Some full text articles may not yet be available without a charge during the embargo (administrative interval).
What is a DOI Number?
Some links on this page may take you to non-federal websites. Their policies may differ from this site.
-
Abstract P = 95–237 days and small semiamplitudeK 1< 11 km s−1. We combined the Be star velocities with prior sdO measurements to obtain mass ratios. A Doppler tomography algorithm shows the presence of the Heii λ 4686 line in the faint spectrum of the hot companion in four of the targets. We discuss the observed line variability and show evidence of phase-locked variations in the emission profiles of HD 157832, suggesting a possible disk spiral density wave due to the presence of the companion star. The stripped companions in HD 113120 and HD 137387 may have a mass larger than 1.4M ⊙, indicating that they could be progenitors of Type Ib and Ic supernovae. -
Wang, Luqian ; Gies, Douglas R. ; Lester, Kathryn V. ; Guo, Zhao ; Matson, Rachel A. ; Peters, Geraldine J. ; Dhillon, Vik S. ; Butterley, Tim ; Littlefair, Stuart P. ; Wilson, Richard W. ; et al ( , The Astronomical Journal)