Childhood and Emotion

Jarzebowski, Claudia; Safley, Thomas Max

doi:10.4324/9781315850870

Cited by 7 publications

(1 citation statement)

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“…From several observations, it is known that the phases of these periodic modulations are directly correlated (Catalano, Kroll, & Leone, 1992). For some CP stars, the phase extrema of the variations coincide with each other (53 Cam;Jarzȩbowski 1960), while some of the extrema occur in the anti-phase for some other stars (CS Vir; Mikulášek et al 2004). On the other hand, in some cases such as HD 83 368 (Polosukhina et al, 1999), the extrema do not take place at the same time even though the periods of all these variations are same.…”

Section: Introduction: Chemically Peculiar Starsmentioning

confidence: 90%

Photometric Variability of the mCP Star CS Vir: Evolution of the Rotation Period

Özuyar

Şener

Stevens

2018

Publ. Astron. Soc. Aust.

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The aim of this study is to accurately calculate the rotational period of CS Vir by using STEREO observations and investigate a possible period variation of the star with the help of all accessible data. The STEREO data that cover five-year time interval between 2007 and 2011 are analyzed by means of the Lomb-Scargle and Phase Dispersion Minimization methods. In order to obtain a reliable rotation period and its error value, computational algorithms such as the Levenberg-Marquardt and Monte-Carlo simulation algorithms are applied to the data sets. Thus, the rotation period of CS Vir is improved to be 9.29572(12) days by using the five-year of combined data set. Also, the light elements are calculated as HJDmax = 2 454 715.975(11) + 9 d · 29572(12) × E + 9 d · 78(1.13) × 10 −8 × E 2 by means of the extremum times derived from the STEREO light curves and archives. Moreover, with this study, a period variation is revealed for the first time, and it is found that the period has lengthened by 0.66(8) s y −1 , equivalent to 66 seconds per century. Additionally, a time-scale for a possible spin-down is calculated around τ SD ∼ 10 6 yr. The differential rotation and magnetic braking are thought to be responsible of the mentioned rotational deceleration. It is deduced that the spin-down time-scale of the star is nearly three orders of magnitude shorter than its main-sequence lifetime (τ MS ∼ 10 9 yr). It is, in return, suggested that the process of increase in the period might be reversible.

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Section: Introduction: Chemically Peculiar Starsmentioning

confidence: 90%