Computer Science
Scientific paper
Jan 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990phdt........38t&link_type=abstract
Thesis (PH.D.)--MASSACHUSETTS INSTITUTE OF TECHNOLOGY, 1990.Source: Dissertation Abstracts International, Volume: 52-05, Secti
Computer Science
3
Binary Stars
Scientific paper
We have studied type II bursts from the Rapid Burster with durations between ~2 sec and ~680 sec. Time-invariant burst profiles occur over limited ranges of burst durations but there is a gradual evolution in burst profiles over the full range of burst durations. With increasing burst duration, the relative length of the approximately flat top of the bursts increases at the expense of the number of the oscillations during burst decay. The spectral evolution in bursts with similar profiles is similar. However, the blackbody color temperature observed at burst maximum increases with increasing bolometric burst flux. We have analyzed observations of the 11 minute coherent modulation in the X-ray flux from 4U 1820-30. Observations made with the Ginga satellite show that the 685 sec period of this system decreases on a time scale of ~ 10^7 years, contrary to the increase expected. Gravitational acceleration of 4U 1820 -30 in the gravitational potential of the cluster, or caused by a distant companion in a hierarchical triple system, are both viable explanations for this apparent discrepancy. We have made X-ray observations of GX5-1 with a Ginga Observatory. High-frequency QPO were observed in both the HB and the NB; low-frequency QPO were observed in the NB simultaneously with the high-frequency QPO. In the low-frequency QPO, we found that the high-energy X -rays lagged the low-energy X-rays by 82.7 +/- 8.4 ms, therefore, confirming a similar result reported earlier. Our simultaneous X-ray/radio observations of GX5 -1 have shown for the first time that radio emission is low when the X-ray source is in the horizontal branch, and the radio emission is high when the X-ray source was in the normal branch. This result is opposite to that found previously in GX17 + 2, Cyg X-2 and Sco X-1, where radio emission is weakest when the X-ray source is in the flaring branch, stronger when in the normal branch, and strongest of all when in the horizontal branch. (Abstract shortened with permission of school.) (Copies available exclusively from MIT Libraries, Rm. 14-0551, Cambridge, MA 02139-4307. Ph. 617-253-5668; Fax 617-253-1690.).
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