Balmer Line Strengths in Two AP Stars: ∊ Ursae Majoris and 73 Draconis

Wood, H. John

doi:10.1086/128074

Cited by 10 publications

(2 citation statements)

References 1 publication

(1 reference statement)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We also note that the rapid variations found by Wood ( 1964 ) and Honeycutt ( 1966 ) were discussed by them using the period given by Rakos. We have computed the phases of Wood's and Honeycutt's observations from equation ( 1) and find that these phenomena occurred roughly in the same part of the Eu n cycle as Wood and Honeycutt stated, so that no change in the interpretation of these phenomena is required.…”

Section: Period and Phasementioning

confidence: 53%

“…More recently, H. J. Wood ( 1964 ) The present investigation was undertaken in 1964 to determine whether, in view of Babcock's comments, the variations reported by Morgan and Durham are still detectable. With Wood's announcement of rapid variations in the hydrogen lines, the program was expanded to include an attempt to detect these photographically with sufficient resolution to determine whether the hydrogen lines were indeed varying, rather than the many metallic lines that are blended with the wings of the Baimer lines, and which are not resolved in the photoelectric work.…”

Section: Photoelectric Photometry Bymentioning

confidence: 89%

See 1 more Smart Citation

Spectrum Variations in the Peculiar A Star 73 Draconis

Bonsack¹,

Markowitz²

1967

PASP

View full text Add to dashboard Cite

Variations in equivalent width and wavelength have been measured for a selection of lines. The equivalent widths of lines of Eu n, Ca h, Sr n, and Ti n are found to vary synchronously with a period of 20*276, in agreement with results reported by Morgan in 1933 and Durham in 1943. We find no evidence for the change in period suggested by Rakos. The wavelengths vary with the same period, but the phase relationship between the intensity and wavelength variation is different for different elements. Rapid deviations from the systematic variations occur in both intensity and wavelength. Rapid changes in the wings of the hydrogen lines discovered photoelectrically by Wood are confirmed, and it is found that the metallic lines blended in the wings do not participate significantly in the variation.

show abstract

Section: Period and Phasementioning

confidence: 53%

Section: Photoelectric Photometry Bymentioning

confidence: 89%

Spectrum Variations in the Peculiar A Star 73 Draconis

Bonsack¹,

Markowitz²

1967

PASP

View full text Add to dashboard Cite

show abstract

Rusian text ignored

1976

Astron Nachr

View full text Add to dashboard Cite

I a~u p -a a~e , I I I e M a x a ILI e M ax u H C K a R ACT p 0 I# u 3~9 e C K a FI 0 6 c e p B a~ o p u FIThe behaviour of the Balmer lines in the spectra of 13 Apstars has been investigated. It was found that all the investigated stars show the variation in the hydrogen line contours, equivalent widths and the variation of Ig ne and lg(N,#) as well. The curves of the equivalent width variations during the period have several maxima and minima whereas the light curves have no more than two maxima and minima. While transiting from one line to another the position of the extremum coincides very seldom.The electron concentration determined for all stars by the Balmer line profiles has the minimum in those placeswhere the spots with the higher concentration ofone or another element aresituated. It is possible that the most intensive spot of the definite chemical element is responsible for the minimum of lg n,. The hydrogen line profiles show that the lines are always wider and deeper at the moment of minimum light than at the moment of its maximum. I n some cases the hydrogen line center has a complex profile. The measurements of the radial velocity of the absorptional peak in the center of the hydrogen lines of H,, Ha. H, show the existence of rapid changes in 17 Com A and HD 224801 with a characteristic time scale equal to 71 minutes and 6 hours, respectively. 13 18 6 10 18 8 10 15 12 33 2a 12 a B OcTanbmx aseanax, aTo nenbax Ob'bmHHTb TomKO UaMenenaeM TemnepaTypu. B meane HD 140728 MenReTcR Becb XOHTYP BOAOPO~HHX JIUHEIB. CpaBnenne KOHTYPOB ~o n o p o~ HHX J I H H H~~ y HD 140728 c K O H T~~~W S~ B O~O P O~H~X J I H H I~~~ mean B aHTepsane B8-A2 He AaeT cosnanenafi BH B OAHOM cnysae; M O~H O cKaaaTb, TO nApa ~o n o p o~n u x nenni mape, name seM y mean macca A0 (PHC. 5). ConocTaBsenae MeCTOnonowemi nmen, onpenenennrJx no nnnam paanamax xmaqecmix aneMemoB, c naMeHenaeM lg n, no-KaamaeT, TO n m i a naxonmcs B Tex MecTax, rge lg ne nonysaeT namenbmee anaseHae. H D 193722. 3~asenae aKBnBanenTrxoi ~~Z I H H BOAOPO~HUX ammiti (H6-HI4) B TeseHHe ~O T O -MeTpn~eCKOrO IIepnOJJa IlOJIylraeT HeCKOJIbKO MaKCHMYMOB El MHHnMyMOB. nOcJIe BburOHa B CBeT pa6OTM J D a = 2440795.38 -+ Id132854 E . Acnanosa a ~p . (1973), IIIeHaixoM VosHen nepnon aseanbl HD 193722, a n e~e m b~ KOTOpOrO PaBnu

show abstract

The spectrum of the Cr star epsilon ursae majoris

Tektunali

1981

Astrophys Space Sci

View full text Add to dashboard Cite

Balmer Line Strengths in Two AP Stars: ∊ Ursae Majoris and 73 Draconis

Cited by 10 publications

References 1 publication

Spectrum Variations in the Peculiar A Star 73 Draconis

Spectrum Variations in the Peculiar A Star 73 Draconis

Rusian text ignored

The spectrum of the Cr star epsilon ursae majoris

Contact Info

Product

Resources

About