Revised list of pulsating stars with ultra-short periods

Halprin, L.; Moon, T. T.

doi:10.1007/bf00650212

Cited by 10 publications

(5 citation statements)

References 13 publications

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“…Here the objects were not required to be extended, although a few of the stars had the confusion flag set to 3 at 12 |xm. Aumann's criteria were similar to ours, namely, that the sources should have been detected at 12 |xm, 25 |xm, and 60 |xm, that they should be associated with stars in the Gliese catalog, and that they (Edwards, 1976) SAO99809: This is a short period 6 Scuti star according to Halprin and Moon (1983).…”

Section: H Selection Criteriasupporting

confidence: 64%

Cool circumstellar matter around nearby main-sequence stars

Walker

Wolstencroft

1988

PASP

132

105

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Stars are presented which have characteristics similar to Vega and other main-sequence stars with cool dust disks, based on the IRAS Point Source Catalog fluxes. The objects are selected to have a 60 |xm/100 |xm ratio similar to Vega, ß Pic, a PsA, and e Eri, and they are also required to show evidence of extension in the IRAS Working Survey Database. The fluxes are modeled using a blackbody energy distribution. The temperatures derived range from 50 K to 650 K. The diameters of the dust disks observed by IRAS are estimated.

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Section: H Selection Criteriasupporting

confidence: 64%

Cool circumstellar matter around nearby main-sequence stars

Walker

Wolstencroft

1988

PASP

132

105

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“…The Pop I counterparts of SX Phe stars are δ Sct variables. Variables with amplitudes as small as a few hundreds of magnitude prevail in the sample of bright δ Sct stars (Halprin & Moon 1983). We predict that the currently conducted surveys of nearby clusters will result in the discovery of many SX Phe stars with very small amplitudes.…”

Section: Discussionmentioning

confidence: 90%

New variable stars in the globular cluster NGC 288

Kałużny

Krzemiński

Nalezyty

1997

Astron. Astrophys. Suppl. Ser.

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Abstract. We report discovery of 3 new faint variables in the globular cluster NGC 288: 2 SX Phe stars and 1 contact binary. Both SX Phe variables are blue stragglers. The contact binary is located below cluster turnoff, slightly to the red of the main sequence. New photometry of 6 previously known variables is also presented. We note that 26 out of a total 43 SX Phe stars identified recently in ω Cen and NGC 288 exhibit V -band light curves with full amplitudes smaller than 0.10 mag. The sample of known SX Phe stars is likely to be significantly incomplete in regard to the low amplitude variables 1 .

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“…Using these cycle-count periods for a large number of stars, Breger (1979) (Breger 1979). Halprin & Moon (1983) found a smaller coefficient of (b-y) , 5.285, and Frolov & Irkaev (1984) gave the equation o Mv = -2.02 log P + 5.39 (b-y)o -1.33 ± Offi.33 (1.2) where coefficients for log P and (b-y) are smaller than o Breger's. This may indicate a smaller slope for the P-L-C relation for Main Sequence pulsators alone.…”

Section: Period and Amplitude Of Variationmentioning

confidence: 92%