VizieR Online Data Catalog: Evolutionary models of cold and low-mass planets (Linder, 2019)
Abstract
The evolutionary calculations presented here were obtained with the evolutionary model described in Jin et al. (2014ApJ...795...65J), which is itself based on the model of planetary evolution of Mordasini et al. (2012A&A...547A.111M,2012A&A...547A.112M). This model describes the planets as consisting of three distinct homogeneous layers, namely a H/He envelope (using the equation of state (EoS) of Saumon et al. 1995ApJS...99..713S), an ice layer (for planets which have accreted outside of the iceline), and a rocky core, which itself consists of silicates and iron. To address the cooling and contraction of very low-mass planets, we have extended the model in regard to two aspects.
COOLING CURVES: The filename: The first number corresponds to the atmospheric model, -2 is for the petitCODE grid, -3 for the HELIOS grid. Then the metallicity is given. There are different models, clear and with clouds. If the model contains clouds, the settling parameter fsed is given. The planetary mass in Earth masses is at the end of the filename. For some masses, also brighter and fainter cases are calculated. These are named with a brighter resp. fainter in the end. The header: The header repeats the file name information, it gives a conversion factor for the luminosity and the column names and units. All the magnitudes are in absolute magnitudes. In the files: The planetary characteristics and magnitudes are given as long as the magnitudes can be calculated, which means as long as the planet is evolving in the logg-temperature of the atmospheric grid. For the cloudy grid, the magnitudes are calculated as long as the planet is above 200K. ISOCHRONES: The filename: Khe first number corresponds to the atmosphric model, -2 is for the petitCODE grid, -3 for the HELIOS grid. Then the metallicity is given. There are different models, clear and with clouds. If the model contains clouds, the settling parameter fsed is given. For some masses, also brighter and fainter cases are calculated. These are named with a brighter resp. fainter in the end. The header: The header repeats the file name information, it gives a conversion factor for the luminosity and the column names and units. All the magnitudes are in absolute magnitudes. In the files: The planetary characteristics and magnitudes are given as long as the magnitudes can be calculated, which means as long as the planet is evolving in the logg-temperature of the atmospheric grid. For the cloudy grid, the magnitudes are calculated as long as the planet is above 200K. (5 data files).- Publication:
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VizieR Online Data Catalog
- Pub Date:
- March 2019
- DOI:
- 10.26093/cds/vizier.36230085
- Bibcode:
- 2019yCat..36230085L
- Keywords:
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- Models: evolutionary;
- Photometry