Modeling the ionizing spectra of H II regions: individual stars versus stellar ensembles
Aims: We study how IMF sampling affects the ionizing flux and emission line spectra of low mass stellar clusters. Methods: We performed 2 × 106 Monte Carlo...
Modeling the photometric and dynamical behavior of Super-Schmidt meteors in the Earth's atmosphere
Faint meteors observed with Super-Schmidt cameras are re-examined in order to assess whether their dynamical and photometric behavior can be described by means...
Modeling the scattering polarization of the solar Ca I 4227 Å line with angle-dependent partial frequency redistribution
Context. The correct modeling of the scattering polarization signals observed in several strong resonance lines requires taking partial frequency redistribution...
Modeling the Stellar Populations in the Canis Major Overdensity: The Relation between the Old and Young Populations
We analyze the stellar populations of the Canis Major stellar overdensity using quantitative color-magnitude diagram (CMD) fitting techniques. The analysis is...
Modeling the Strongest Silicate Emission Features of Local Type 1 AGNs
We measure the 10 and 18 μm silicate features in a sample of 67 local (z < 0.1) type 1 active galactic nuclei (AGN) with available Spitzer spectra dominated by...
While sunspots are easily observed at the solar surface, determining their subsurface structure is not trivial. There are two main hypotheses for the subsurface...
Modeling the thermal conduction in the solar atmosphere with the code MANCHA3D
Context. Thermal conductivity is one of the important mechanisms of heat transfer in the solar corona. In the limit of strongly magnetized plasma, it is...
Modeling the Unresolved NIR-MIR SEDs of Local (z < 0.1) QSOs
To study the nuclear (≲1 kpc) dust of nearby (z < 0.1) quasi-stellar objects (QSOs), we obtained new near-infrared (NIR) high angular resolution (~0.″3)...