Water in Sunspots and Stars

Bernath, P. F.

doi:10.1017/s1539299600012867

Cited by 2 publications

(1 citation statement)

References 19 publications

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“…Faculae and plages are characterized on the Sun by magnetic field strengths less than the photospheric gas equipartition value of ∼1,500 G. Field strengths in sunspot umbrae generally range from ∼ 2,000-4,000 G and with temperatures in the broad range of ∼ 50-80% of the solar effective temperature. The identification of water vapor lines in sunspot umbral spectra is consistent with the occurrence of low temperatures ∼3,000 K (28). The filling factor of the quiet facular network In transiting exoplanet transmission spectroscopy the light source is the chord defined by the planet's projection, but its spectrum is not directly observable.…”

Section: Solar and Stellar Heterogeneitysupporting

confidence: 56%

Understanding Stellar Contamination in Exoplanet Transmission Spectra as an Essential Step in Small Planet Characterization

Apai,

Rackham,

Giampapa

et al. 2018

Preprint

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Transmission spectroscopy during planetary transits is expected to be a major source of information on the atmospheres of small (approximately Earth-sized) exoplanets in the next two decades. This technique, however, is intrinsically affected by stellar spectral contamination caused by the fact that stellar photo-and chromospheres are not perfectly homogeneous. Such stellar contamination will often reach or exceed the signal introduced by the planetary spectral features. Finding effective methods to correct stellar contamination -or at least to quantify its possible range -for the most important exoplanets is a necessary step for our understanding of exoplanet atmospheres. This will require significantly deepening our understanding of stellar heterogeneity, which is currently limited by the available data.

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Section: Solar and Stellar Heterogeneitysupporting

confidence: 56%