[논문]SUN FLUX VARIATIONS DUE TO ORBITING PLANETS: THE SOLAR SYSTEM AS A NON-COMPACT PLANETARY SYSTEM

Barbier, Hugo; Lopez, Ericson D.; Tipan, Bryan; Vasconez, Christian L.

doi:10.5303/jkas.2020.53.3.69

SUN FLUX VARIATIONS DUE TO ORBITING PLANETS: THE SOLAR SYSTEM AS A NON-COMPACT PLANETARY SYSTEM 원문보기

Journal of the Korean astronomical society = 천문학회지, v.53 no.3, 2020년, pp.69 - 75

Barbier, Hugo (Departamento de Fisica, Escuela Politecnica Nacional) , Lopez, Ericson D. (Departamento de Fisica, Escuela Politecnica Nacional) , Tipan, Bryan (Departamento de Fisica, Escuela Politecnica Nacional) , Vasconez, Christian L. (Departamento de Fisica, Escuela Politecnica Nacional)

Abstract ▼ AI-Helper

We study the photometric phase curves for the planets of our solar system which can be considered as a prototypical non-compact planetary system. We focus on modeling the small variations caused by three effects: reflection, ellipsoidal, and Doppler beaming. Theoretical predictions for these photometric variations are proposed, considering a hypothetical external observer. Unlike similar studies of multi-planetary systems, the physical and geometrical parameters for each planet of the solar system are well-known. Therefore, we can accurately evaluate the relationships that shape the planetary light curves for a fictitious external observer. Our results suggest that, for all planets, the ellipsoidal effect is very weak while the Doppler beaming effect (DBE) is, in general, dominant. In fact, the DBE seems to be the principal cause of variations of the light curves for the planets of the solar system. However, for Mercury and Venus the Doppler beaming and reflection effects have similar amplitudes. The phase curves obtained for the planets of the solar system show new interesting features of interest for the study of other non-compact planetary systems.

주제어

표/그림 (6)

그림 Figure 1. Logarithmic relative flux variation (ΔF/F₀) as function of time for the eight planets of the solar system.
그림 Figure 2. The direct sum of the three eects that contribute to the total (ΔF=F₀)_tot for each planet.
그림 Figure 3. Decay of the amplitude of each eect for a Jupiter-type planet, as function of distance to the host star a.
표 Table 1 Solar system planets parameters (Cox 2000)
표 Table 2 Sun parameters (Cox 2000)
표 Table 3 Maximum light-curve variations for the solar system planets

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문제 정의

2013). With this in mind, our work is focused on studying the phase Corresponding author: H. Barbier 1See, e.g., http://exoplanetarchive.ipac.caltech.edu curves of non-compact systems. We compute the “tiny” photometric variations caused by the reflection, ellipsoidal and the Doppler beaming effects.

제안 방법

In this study, we have evaluated the phase curves for the eight planets of the Solar System. The tiny variations of the stellar flux due to the Doppler beaming, reflection, and ellipsoidal effects have been studied from the point of view of a fictitious observer located outside of this non-compact system but aligned with the ecliptic plane.

대상 데이터

For our study, we analyze the eight solar system planets: Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, and Neptune. We do not consider trans-Neptunian objects or small solar system bodies, due to their negligible effects on the global system dynamics.

성능/효과

One of the most important conclusions of this study is that, for a hypothetical observer outside the solar system, the Doppler-beaming effect is the most relevant. This effect is the easiest one to be detected, especially for the outer planets.

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