Tag: metallicity

The relation between stellar metallicity and presence of giant planets in intermediate massive stars described in the study: “Intermediate-mass stars and the origin of the gas-giant planet-metallicity correlation” of J. Maldonado (INAF-OAPA)

Ricerca

As of today (February 2025), out of the 5834 identified exoplanets, only about 5% orbit stars with masses between 1.5 and 3.5 solar masses (intermediate-mass stars). This is likely due to specific difficulties in exoplanet detection techniques, difficulties that are not encountered for lower-mass stars. For example, since they are more luminous than lower-mass stars, the transit depth (i.e., the

» Read more
, , , , , ,

There is no relation between age and metallicity of the stars in the Solar neighbourhood. The study: “Constraining the solar neighbourhood age-metallicity relation from white dwarf-main sequence binaries” of A. Rebassa-Mansergas (Universitat Politècnica de Catalunya) recently appeared on MNRAS

Ricerca

After the Big Bang, the Universe contained only hydrogen, helium, and a very small fraction of lithium. After that, stars, mainly the most massive ones, were responsible for the chemical enrichment of the Universe. In fact, stars produce energy by synthetizing chemical elements in their cores. These elements are then redistributed in the interstellar medium when stars end their evolution.

» Read more
, , , , , , , ,

Stellar chemical composition and planetary formation. The study “Connecting substellar and stellar formation. The role of the host star’s metallicity” of J. Maldonado (INAF-OAPA) recently appeared on A&A

Ricerca

To date, about 4000 exoplanets (planets orbiting around other stars) have been confirmed. Stars hosting planets and sub-stellar companions span a wide range of stellar parameters and even evolutionary phases. For this reason, several studies have been focused on the connection between stellar parameters and the possibility to host planets or sub-stellar companions such as brown dwarfs.   In particular,

» Read more
, , ,