NSF Org:	AST Division Of Astronomical Sciences
Recipient:	GEORGIA STATE UNIVERSITY
Initial Amendment Date:	March 4, 1992
Latest Amendment Date:	March 4, 1992
Award Number:	9115121
Award Instrument:	Standard Grant
Program Manager:	Jane Russell AST  Division Of Astronomical Sciences MPS  Directorate for Mathematical and Physical Sciences
Start Date:	March 1, 1992
End Date:	August 31, 1995 (Estimated)
Total Intended Award Amount:	$90,000.00
Total Awarded Amount to Date:	$90,000.00
Funds Obligated to Date:	FY 1992 = $90,000.00
History of Investigator:	Douglas Gies (Principal Investigator)
Recipient Sponsored Research Office:	Georgia State University 33 GILMER ST SE ATLANTA GA  US  30303-3044 (404)413-3500
Sponsor Congressional District:	05
Primary Place of Performance:	DATA NOT AVAILABLE
Primary Place of Performance Congressional District:
Unique Entity Identifier (UEI):	SNQ6M7S6TK89
Parent UEI:
NSF Program(s):	STELLAR ASTRONOMY & ASTROPHYSC
Primary Program Source:
Program Reference Code(s):
Program Element Code(s):	121500
Award Agency Code:	4900
Fund Agency Code:	4900
Assistance Listing Number(s):	47.049

ABSTRACT

The spectral absorption lines of hot, rapidly rotating "B" type stars show traveling "bumps" which travel across the lines with time. Although these bumps were first thought to move periodically in a predictable way, leading to an interpretation that traveling waves (nonradial pulsations) were responsible, new data indicate that the bumps are often missing. In order to judge whether this apparent unpredictability is caused by the "beating" of different pulsation modes or by an aperiodic phenomenon, long strings of spectroscopic data are needed. In the past long "campaigns" have been difficult to undertake because of practical scheduling and allocation problems at national facilities. In early 1992 Georgia State will put into operation its new spectroscopic "Multi- Telescope Telescope. This facility will have a large effective light gathering power and a Charged-Couple Device detector and will permit the PI to obtain large amounts of data to examine the frequency of the "profile bump" phenomenon in rapidly rotating B stars and to ascertain its periodic nature. The PI also believes that the large database assembled will enable him to determine whether nonradial pulsations are responsible for episodic mass loss in the enigmatic group of rapidly rotating "Be" stars.

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