2003
DOI: 10.1051/0004-6361:20030401
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Modelling the rotational modulation of the Sun as a star

Abstract: Abstract.We analyse the time variability of the total solar irradiance (TSI) as measured by VIRGO/SoHO in order to model the variability of the Sun as a star. Apart from the phases near the minimum at the beginning of activity cycle 23, the period of the rotational modulation is significantly different from the solar synodic period as a consequence of the growth and decay of active regions on time scales shorter than a solar rotation. In order to model the variability of the TSI, we have considered the contrib… Show more

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Cited by 107 publications
(177 citation statements)
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“…The timescales of the stellar flux variability and the transit are generally quite different, since the former may range from weeks to months as in the case of the Sun (Lanza et al 2003(Lanza et al , 2007, while the latter has a duration ranging from a few hours to a few tens of hours. However, there are situations in which the timescales can be comparable, e.g., for a young Sun-like star with a rotation period of, say, 1-2 days transited by a planet at the distance of ∼1 AU, whose transit duration is of the order of ∼10-15 h. In this case, a discrimination of the origin of the light dip based on timescales is infeasible, while our approach is still applicable if simultaneous multiwavelength observations are available.…”
Section: Influence Of Stellar Activity On Stellar Colours and The Chamentioning
confidence: 99%
“…The timescales of the stellar flux variability and the transit are generally quite different, since the former may range from weeks to months as in the case of the Sun (Lanza et al 2003(Lanza et al , 2007, while the latter has a duration ranging from a few hours to a few tens of hours. However, there are situations in which the timescales can be comparable, e.g., for a young Sun-like star with a rotation period of, say, 1-2 days transited by a planet at the distance of ∼1 AU, whose transit duration is of the order of ∼10-15 h. In this case, a discrimination of the origin of the light dip based on timescales is infeasible, while our approach is still applicable if simultaneous multiwavelength observations are available.…”
Section: Influence Of Stellar Activity On Stellar Colours and The Chamentioning
confidence: 99%
“…3.3. Since there are many free parameters in the ME model is large, for this specific application we make use of the model of Lanza et al (2003), which fits the light curve by assuming only three active regions to model the rotational modulation of the flux plus a uniformly distributed background to account for the variations in the mean light level. This procedure is the same as used to fix the value of Q in the cases of CoRoT-2, CoRoT-4, CoRoT-7, and CoRoT-6 (cf.…”
Section: Spot Modellingmentioning
confidence: 99%
“…The simple three-spot model of Lanza et al (2003) has been applied to fit the individual intervals to reduce the number of free parameters. The optimal N f is given by the minimum value that allows us a good fit to the light curve as measured by the χ 2 statistics.…”
Section: Model Parametersmentioning
confidence: 99%
“…This is allowed because chromospheric active regions and activity complexes are remarkably long-lived in comparison with photospheric spots having a mean lifetime of 50−80 days vs. ∼10−15 days, respectively (cf. Donahue et al 1997a;Lanza et al 2003). As a matter of fact, a similar approach based on photospheric sunspots was not successful because of the random longitude appearance and short lifetime of individual sunspot groups (Labonte 1984).…”
Section: Introductionmentioning
confidence: 99%