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TAU PEGASIA FOURIER REPRESENTATION OF LINE-PROFILE VARIATIONS

by: E. J. KENNELLY, G. A. H. WALKER, and W. J. MERRYFIELD

In: ASTROPHYSICAL JOURNAL, Vol. 400, Nr. 2 (1992) , p. L71--L74.

Abstract

The complex line-profile variations, probably caused by nonradial pulsations, in the spectrum of the rapidly rotating delta Scuti star tau Peg are analyzed with a novel two-dimensional Fourier transform technique. It resolves the oscillations in temporal frequency nu and apparent azimuthal order m. The two-dimensional Fourier spectrum resembles the 1, nu diagrams generated for the Sun. Advantages of the technique are 1 both frequency and mode of the oscillations are determined directly; 2 complex variations in the line profiles are resolved into individual modes; 3 modes of both high and low degree are resolved. For tau Peg, we identify four apparent modes having Absolute value of m congruent-to 3, 7, 11, and 15. After correcting for rotation, most of the modes have frequencies of approximately 17 cycles day-1. Assuming Teff congruent-to 8000 K and L congruent-to 40 L., all of the modes fall within the range of frequencies theoretically predicted to be unstable.

BibTeX record

@article{KENNELLY1992,
  abstract = {The complex line-profile variations, probably caused by nonradial
	pulsations, in the spectrum of the rapidly rotating delta Scuti star
	tau Peg are analyzed with a novel two-dimensional Fourier transform
	technique. It resolves the oscillations in temporal frequency nu
	and apparent azimuthal order m. The two-dimensional Fourier spectrum
	resembles the (1, nu) diagrams generated for the Sun. Advantages
	of the technique are (1) both frequency and mode of the oscillations
	are determined directly; (2) complex variations in the line profiles
	are resolved into individual modes; (3) modes of both high and low
	degree are resolved. For tau Peg, we identify four apparent modes
	having Absolute value of m congruent-to 3, 7, 11, and 15. After correcting
	for rotation, most of the modes have frequencies of approximately
	17 cycles day-1. Assuming T(eff) congruent-to 8000 K and L congruent-to
	40 L., all of the modes fall within the range of frequencies theoretically
	predicted to be unstable.},
  added-at = {2009-11-03T20:21:25.000+0100},
  author = {KENNELLY, E. J. and WALKER, G. A. H. and MERRYFIELD, W. J.},
  biburl = {http://www.bibsonomy.org/bibtex/2a1684b2797505679b3aacbbb5dd59ab6/svance},
  citedreferences = {BREGER M, 1989, ASTRON ASTROPHYS, V214, P209 ; BREGER M, 1991, ASTRON ASTROPHYS, V250, P107 ; CAMPOS AJ, 1980, APJ, V238, P667 ; CRAWFORD DL, 1979, ASTRON J, V84, P1858 ; DZIEMBOWSKI WA, 1990, LECT NOTE PHYS, V367, P359 ; GIES DR, 1988, ASTROPHYS J, V326, P813 ; HAUCK B, 1980, ASTRON ASTROPHYS SUP, V40, P1 ; KAMBE E, 1988, PUBL ASTRON SOC JPN, V40, P313 ; KENNELLY EJ, 1991, PUBL ASTRON SOC PAC, V103, P1250 ; KENNELLY EJ, 1992, IN PRESS ASP C SER ; KENNELLY EJ, 1992, UNPUB ; MATTHEWS JM, 1985, PUBL ASTRON SOC PAC, V97, P841 ; MERRYFIELD WJ, 1992, UNPUB ; MICHEL E, 1990, ASP C SER, V11, P332 ; PHILIP AGD, 1979, ASTRON J, V84, P1743 ; SMITH MA, 1982, ASTROPHYS J, V254, P242 ; UNNO W, 1989, NONRADIAL OSCILLATIO, P19 ; VOGT SS, 1983, ASTROPHYS J, V275, P661 ; WALKER GAH, 1987, APJ, V320, L139 ; YANG S, 1986, PUBL ASTRON SOC PAC, V98, P1156},
  interhash = {26282ecaf43b16a5ff876acfa0cc881b},
  intrahash = {a1684b2797505679b3aacbbb5dd59ab6},
  journal = {ASTROPHYSICAL JOURNAL},
  keywords = {DELTA-SCUTI NONRADIAL OSCILLATIONS; STARS; VARIABILITY},
  number = 2,
  owner = {svance},
  pages = {L71--L74},
  timestamp = {2009-11-03T20:21:25.000+0100},
  title = {TAU PEGASIA FOURIER REPRESENTATION OF LINE-PROFILE VARIATIONS},
  volume = 400,
  year = 1992
}

Endnote record

%0 Journal Article
%1 KENNELLY1992
%A KENNELLY, E. J.
%A WALKER, G. A. H.
%A MERRYFIELD, W. J.
%D 1992
%J ASTROPHYSICAL JOURNAL
%K 
%N 2
%P L71--L74
%T TAU PEGASIA FOURIER REPRESENTATION OF LINE-PROFILE VARIATIONS
%V 400
%X The complex line-profile variations, probably caused by nonradial
	pulsations, in the spectrum of the rapidly rotating delta Scuti star
	tau Peg are analyzed with a novel two-dimensional Fourier transform
	technique. It resolves the oscillations in temporal frequency nu
	and apparent azimuthal order m. The two-dimensional Fourier spectrum
	resembles the (1, nu) diagrams generated for the Sun. Advantages
	of the technique are (1) both frequency and mode of the oscillations
	are determined directly; (2) complex variations in the line profiles
	are resolved into individual modes; (3) modes of both high and low
	degree are resolved. For tau Peg, we identify four apparent modes
	having Absolute value of m congruent-to 3, 7, 11, and 15. After correcting
	for rotation, most of the modes have frequencies of approximately
	17 cycles day-1. Assuming T(eff) congruent-to 8000 K and L congruent-to
	40 L., all of the modes fall within the range of frequencies theoretically
	predicted to be unstable.