Radial Velocity Variations in 69 Orionis

Bossi, M.; Guerrero, G.; Mantegazza, L.

doi:10.1007/978-94-009-8565-0_32

Cited by 8 publications

(15 citation statements)

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“…Abbreviations L, R, O, and S denote (by black dots) the presence of variations on a time scale of years and months (L), days or fraction of day (R), orbital (O) and sudden light changes (S), respectively References to Table: m 1 in V were detected by . Bossi et al (1989) confirmed the variations on a short time-scale, but not their large amplitude. They interpreted them as multiperiodic nonradial pulsations.…”

Section: Hd 21551 (Hr 1051)mentioning

confidence: 60%

UBV photometry of Be stars at Hvar: 1972–1990

Pavlovski¹,

Harmanec

Božić³

et al. 1997

Astron. Astrophys. Suppl. Ser.

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Abstract. A summary of results of the systematic UBV photoelectric monitoring of bright northern Be stars carried out at the Hvar Observatory between 1972 and 1990 is presented. Altogether, 76 Be stars of all luminosity classes were observed and 13 848 UBV measurements secured. Simultaneously, 9 648 UBV measurements of 48 check stars (most of them of early spectral types) were obtained. A careful transformation of all observations into the standard Johnson system allowed detection and monitoring of even very mild long-term light and colour variations of these objects. Almost all early-type Be stars in the sample turned out to be variable. For several stars phase-locked light variations related to their binary nature were established. Sudden brightenings, on a time scale of a few days, were detected for o Cas and QR Vul.

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Section: Hd 21551 (Hr 1051)mentioning

confidence: 60%

UBV photometry of Be stars at Hvar: 1972–1990

Pavlovski¹,

Harmanec

Božić³

et al. 1997

Astron. Astrophys. Suppl. Ser.

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“…Photometric variations were also studied by Bossi & Guerrero (1989), Percy et al (1994) .85, and by Guo et al (1995).…”

Section: Light and Colour Changesmentioning

confidence: 99%

Properties and nature of Be stars

Ruždjak

Božić

Harmanec

et al. 2009

A&A

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Context. One way to understand the still mysterious Be phenomenon is to study the time variations of particular Be stars with a long observational history. ζ Tau is one obvious candidate. Aims. Using our rich series of spectral and photometric observations and a critical compilation of available radial velocities, spectrophotometry of Hα, and UBV photometry, we characterize the pattern of time variations of ζ Tau over about a century. Our goal is to find the true timescales of its variability and confront them with the existing models related to various aspects of the Be phenomenon. Methods. Spectral reductions were carried out using the IRAF and SPEFO programs. The HEC22 program was used for both photometric reductions and transformations to UBV. Orbital solutions were derived with the latest publicly available version of the program FOTEL, period analyses employed both the PDM and Fourier techniques -programs HEC27 and PERIOD04.

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“…It was first observed by Breger (1970) for two nights in 1968 and 1969. Later, Bossi et al in (1977) (BGM) observed this star for four nights separated 35 days; furthermore, only two of these nights are longer than the assumed period, therefore we worked mainly with their longest nights, HJD 2443173 and 203. A periodogram analysis of the first three nights led them to derive a period of 0.0534d; they reported that the last and the longest night did not fit this frequency but they found more and different frequencies from the analysis of this night: a main peak at 0.059d, and another much less marked peak at 0.068d; however, the 0.0534d component seemed to have disappeared.…”

Section: Resultsmentioning

confidence: 99%

“…Since they didn't report their observations, gross values of their photometry were obtained directly from their reported light curves. The obtained data of this star in 1982 consisted of two consecutive nights, separated from that of Bossi et al (1977) by five years: therefore, a separate analysis of each season was carried out, and no attempt to phase lock was considered.…”

Section: Resultsmentioning

confidence: 99%

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Photoelectric photometry and period analysis of selected Delta Scuti stars in Praesepe

Peña¹,

Peniche²,

Hobart³

et al. 1998

Astron. Astrophys. Suppl. Ser.

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Abstract. Photoelectric photometry of seven Delta Scuti stars in Praesepe was secured. Three of them were observed simultaneously at observatories located at different longitudes. Period analysis has been carried out for each star with different computing packages and the results compared to those in the literature. Their physical characteristics have been determined from the Strömgren photometry and theoretical and empirical calibrations.

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Radial Velocity Variations in 69 Orionis

Cited by 8 publications

References 1 publication

UBV photometry of Be stars at Hvar: 1972–1990

UBV photometry of Be stars at Hvar: 1972–1990

Properties and nature of Be stars

Photoelectric photometry and period analysis of selected Delta Scuti stars in Praesepe

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