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Guy Boistel

Publications and source records attributed to Guy Boistel.

8 recordsLinked to original sources

New O-Cs for the Classical Cepheids RY Cas and V Lac over a Century (1873-2022)

We give here new O-C diagrams of the two classical Cepheids RY Cas and V Lac, established on a large basis of times of maximum of light, which covers more than a century. These two Cepheids present a variation of their period for which it is possible to calculate an annual rate. This rate equals +1.86 s/yr for RY Cas and -0.81 s/yr for V Lac. Based on these two new O-C diagrams neither of them seems to show any association to a binary system.

astro-ph.SR

A new value of the period of the classical Cepheid RT Aur on the basis of 456 times of maximum, 1897-2023

The present study collects 456 new times of maximum light of the classical Cepheid RT Aur, covering the period from 1897 to 2022. The O-C diagram resulting from these observations shows that the period given by the GCVS has to be corrected. It results that no strong period variation is found. However, the observed O-C residuals show a long term periodic trend. In the hypothesis of RT Aur being in a binary system, an orbit cannot be deduced from the available astrophysical data.

astro-ph.SR

Period variation of the classical Cepheid SV Vulpeculae over a century (1913-2022)

This study analyzes 338 new times of visual, CCD, photoelectric and photographic maxima of the classical Cepheid SV Vul. The corresponding observations were made between 1913 and 2022. On this new and large observational basis, the period variations of this star of major astrophysical interest are re-visited. Without contradicting the theory or previous studies, we show that visual observations are important for a long-term monitoring of the period variations of well-selected bright Cepheids. This study establishes the period rate of change of SV Vul at -250 s/yr. Its period is currently shorter than 45 days.

astro-ph.SR

Photometric survey of the red giant V449 Cygni over half a century (1974 to 2022). A semi-regular variable star with a period of ~54 days

This study sums up a major part of the red giant V449 Cygni measurements for the years 1974 through 2022, obtained by visual and CCD GEOS observers, the Unione Astrofili Italiani, and various automatized telescopes. It appears that the light variations of V449 Cyg in the years 1970-1990 corresponded more to an L-type star according to the GCVS classification, with irregular amplitude variations, sometimes marked by a quasi-periodicity of about 100 days. Since the mid-1990s, these variations have become more regular, with an amplitude of about 0.7 magnitude in V, and a period of about 54,1 days, as shown by various period search routines applied to the best recent CCD series. A longer period of about 2000 days is possible to describe the long term variation of V449 Cyg. Therefore, V449 Cyg appears to be an SRB-type star.

astro-ph.SR

Comprendre l atmosphere du Soleil et celles des etoiles variables a la fin du 19e siecle or, Understanding the Sun and variable stars atmospheres at the end of the 19th Century

Guy Boistel questions the Sun / variable stars analogy at the heart of the work of Dutch astronomer Albert Brester. The problem of interdisciplinarity appears in the objectification of the Sun at the end of the 19th century: it is by mixing astronomy, physics and chemistry that Brester tried to apply knowledge of the solar atmosphere to the understanding of variable stars, a fairly confidential field of study still at that time.

physics.hist-ph

Nouvelle theorie des taches du Soleil, by E. Pezenas (1692-1776). A fully annoted edition of a manuscript

The manuscript New Theory of Sunspots was identified and attributed to the Jesuit astronomer and hydrographer from Marseille Esprit Pezenas (1692-1776) during the year 2002, during the systematic search for papers concerning him in the various French funds. The manuscript, in large part unpublished, New Theory of Sunspots was written by astronomer and professor of Marseilles Jesuit hydrography, Father Esprit Pezenas (1692-1776). The text was composed and revised between the years 1766 and 1772. In this manuscript, of which we are going to study the conditions of its composition, P. Pezenas gives one of the last geometric methods, related graphical methods, allowing the inclination of the Sun's equator to be deduced on ecliptic, using three observations of a sunspot, at given times, and in taking into account the movement of the Earth with respect to the Sun during the duration of observations. This text contains all the digital elements allowing to follow and understand the application of geometric processing methods of observations and observation techniques mentioned above in the introduction: passages of edges and Sun spots at the meridian, use of objective micrometers and wire micrometers. At detour of his calculations, Father Pezenas announces a duration of about 26 days and 9 hours for the rotation of the Sun around its axis, comments on and corrects some observation data published in Le Monnier's Heavenly History.

physics.hist-ph

AY Peg, a large amplitude Algol-type star

The present paper gives new elements for the light variations of the EA variable star AY Peg, on the basis of new times of minimum performed visually and with ccd by members of GEOS between 1985 and 2018, and the ASAS-SN set of data available. On one hand, we can establish a new ephemeris with a possible quadratic term, and on the other hand, the amplitude of the primary minimum appears much deeper than the one given in GCVS. AY Peg varies between 13.1 and 15.6 magnitude at its primary eclipse.

astro-ph.SR