Spectral Energy Distribution of 100 stars [Dataset]
Spectral Energy Distribution of 100 stars [Dataset]
The table provides the Spectral Energy Distribution (SED) of 100 stars, modeled using coronal and transition region data as described in Section 3 of the paper. First column represent the Wavelength, in angstroms, and the rest of columns are density flux at 1 a.u. in units of erg/s/cm^2^/{AA}. Atomic data from ATOMDB v3.0.9 (APED, Smith et al. 2001ApJ...556L..91S). This SED represents only the contribution from material at temperatures higher than 10000K. Photospheric contribution should be considered for wavelengths higher than ~1250{AA} in F-M stars, and even shorter wavelengths for A stars (e.g. Kelt-9). The columns of the density flux have their (SIMBAD-compatible) stellar names in the heading.
Peer reviewed
Planets and satellites: general, Stars, late-type, Exoplanets, Planets and satellites: atmospheres, Ultraviolet: planetary systems, Stars: coronae, X-rays: stars, Stars, double and multiple
Planets and satellites: general, Stars, late-type, Exoplanets, Planets and satellites: atmospheres, Ultraviolet: planetary systems, Stars: coronae, X-rays: stars, Stars, double and multiple
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