Simulations of giant impacts between 0.2-4 Earth-mass planets yield post-impact luminosities of 5e-5 to 0.1 L_sun cooling over 1-2000 days, predicting 0-14 detections in Gaia DR4 and a comparable number in LSST.
On the use of Gaia magnitudes and new tables of bolometric corrections
2 Pith papers cite this work. Polarity classification is still indexing.
2
Pith papers citing it
abstract
The availability of reliable bolometric corrections and reddening estimates, rather than the quality of parallaxes will be one of the main limiting factors in determining the luminosities of a large fraction of Gaia stars. With this goal in mind, we provide Gaia G, BP and RP synthetic photometry for the entire MARCS grid, and test the performance of our synthetic colours and bolometric corrections against space-borne absolute spectrophotometry. We find indication of a magnitude-dependent offset in Gaia DR2 G magnitudes, which must be taken into account in high accuracy investigations. Our interpolation routines are easily used to derive bolometric corrections at desired stellar parameters, and to explore the dependence of Gaia photometry on Teff, log(g), [Fe/H], alpha-enhancement and E(B-V). Gaia colours for the Sun and Vega, and Teff-dependent extinction coefficients, are also provided.
years
2026 2representative citing papers
citing papers explorer
-
Can giant impacts be directly detected in other star systems?
Simulations of giant impacts between 0.2-4 Earth-mass planets yield post-impact luminosities of 5e-5 to 0.1 L_sun cooling over 1-2000 days, predicting 0-14 detections in Gaia DR4 and a comparable number in LSST.
- Observational Signatures and Constraints on the Intermediate Neutron-Capture Process. The Case of the CEMP star TYC 6044-714-1 (RAVE J094921.8-161722)