Rotation of solar-like main sequence stars

Stępień, K.; Geyer, E. H.

doi:10.1051/aas:1996141

Cited by 9 publications

(11 citation statements)

References 16 publications

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“…We have found about 80 stars with measured calcium emission flux and about 40 with magnesium emission fluxes. Our main sources of data were the papers by Stȩpień (1994), Saar & Brandenburg (1999) and Messina et al (2001), with a couple of periods taken from Stȩpień & Geyer (1996). References to original determinations of rotation periods and chromospheric fluxes can be found in the first three papers.…”

Section: Observed Magnetic Filling Factorsmentioning

confidence: 99%

Acoustic and magnetic wave heating in stars

Fawzy

Stępień

Ulmschneider

et al. 2002

A&A

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Abstract. Theoretical chromospheric models described in the two previous papers of this series are used to study the relationship between the chromospheric emission and the filling factor. This theoretically determined relationship shows that the chromospheric emission flux in Ca II (H+K) is approximately proportional to the square root of the magnetic filling factor at the stellar surface. To relate the filling factor to stellar rotation rate, we compare the theoretical fluxes with observations of stars with known rotation period. The comparison shows that the Rossby number is probably a more appropriate measure of the rotation influence on activity of main-sequence stars than the rotation period. Our theoretical Mg II (h+k) and Ca II (H+K) emission fluxes are also found to be well correlated, which is in a good agreement with the observational data.

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Section: Observed Magnetic Filling Factorsmentioning

confidence: 99%

Acoustic and magnetic wave heating in stars

Fawzy

Stępień

Ulmschneider

et al. 2002

A&A

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“…Each given measurement at time t which does not show There is no long-term variation for these two stars. Bottom panel shows the periodic variation detected for HD 38392 with a period of 21.4 days corresponding to its rotational period (Stepień & Geyer 1995) this variation allows to eliminate the period P 1 given by the time difference between the measurement and the date November 10: P = P 1 = t − t 11/10/1981 . In fact, considering that if this event had occurred again, it would have been detectable during one day (which is a very conservative assumption), each measurement allows to eliminate the range of period P 1 plus or minus half a day.…”

Section: Constraints On Future β Pictoris Observationsmentioning

confidence: 99%

A three-year Strömgren photometric survey of suspected β Pictoris-like stars

Nitschelm

Vidal‐Madjar

Ferlet

et al. 2000

Astron. Astrophys. Suppl. Ser.

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Abstract. We carried out a Strömgren photometric survey of thirteen southern bright stars, including β Pictoris itself, during three years, d'Astrophysique de Paris, in order to detect possible weak photometric variations. β Pictoris presents a small long-term variation with a change of brightness by −2.1 10 −3 mag per year, over about two years from beginning of 1996, a situation relatively similar to the one about 18 years ago. Among the other stars, only HD 38392 presents weak photometric variations with a period of 21.4 days, probably related to the star rotation period. The negative result concerning photometric variations of all other stars suggests that those stars are actually really stable and strengthens the reality of the variations discovered in the case of β Pictoris and HD 38392.

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“…Values of , the logarithmic ratio of the chro-R HK mospheric luminosity in the calcium H and K lines to the total photospheric emission, are taken from Soderblom (1985), Soderblom & Mayor (1993a), Henry et al (1996), and Baliunas et al (1996). Rotation periods are from Noyes et al (1984), Henry, Fekel, & Hall (1995), Donahue, Saar, & Baliunas (1996), Stepień & Geyer (1996), and Güdel et al (1997a).…”

Section: Sin Fbfmentioning

confidence: 99%

Nearby Young Solar Analogs. I. Catalog and Stellar Characteristics

Gaidos

1998

PUBL ASTRON SOC PAC

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ABSTRACT. We present a catalog of 38 young solar analogs within 25 pc, stars that are uniquely well suited for observations of their circumstellar environments to improve our understanding of conditions within the solar system during the Hadean/early Archean eons (prior to 3.8 Gyr ago). These G and early K stars were selected from the Hipparcos astrometric catalog based on lack of known stellar companions within 800 AU, bolometric luminosities close to that of the zero-age Sun and consistent with the zero-age main sequence, and ROSAT X-ray luminosities commensurate with the higher rotation rate and level of dynamo-driven activity in solar-mass stars less than 0.8 Gyr old. While many of these objects have been previously identified, this sample is novel in two respects: The selection criteria specifically consider the planetary environment, and the selection is uniform and all-sky. The X-ray emission from these young analogs is spectrally soft and consistent with a coronal origin. Calcium H and K emission, rotation periods, lithium abundances, and kinematics support an age range of 0.2-0.8 Gyr for most of these stars. Three stars have exceptionally high space motions with respect to the local standard of rest and may be old disk or halo stars that are anomalously X-ray luminous.

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Rotation of solar-like main sequence stars

Cited by 9 publications

References 16 publications

Acoustic and magnetic wave heating in stars

Acoustic and magnetic wave heating in stars

A three-year Strömgren photometric survey of suspected β Pictoris-like stars

Nearby Young Solar Analogs. I. Catalog and Stellar Characteristics

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