Constraining the stellar energetic particle flux in young solar-like stars

Young stellar populations in the solar neighbourhood

Stellar X-ray surveys play an important role in understanding the star formation history in our Galaxy in the last billion years (the scale time of coronal activity evolution). In particular, the comparison of observed counts in a given sky direction with predictions by Galactic models can put constraints on the spatial distribution and stellar birthrate of stellar populations. We present the r...

Tracing the Evolution and Impact of the Stellar Winds of Solar-Like Stars

Comparison of geosynchronous energetic particle flux responses to solar wind dynamic pressure enhancements and substorms

[1] Geosynchronous energetic particle fluxes are used to examine the differences and similarities between the particle disturbances due to an enhancement in solar wind dynamic pressure Pdyn and those caused by substorms. Disturbances are also distinguished by IMF conditions. First, for not strongly southward IMF conditions (weakly southward or northward IMF), we find that the magnetospheric com...

Moments of energetic particle distributions in the solar atmosphere

This paper describes a theory that provides a direct link between observable properties of energetic particle distributions and the unobservable properties of the initial distributions. A general approach is first outlined and then applied to the specific situation of collisional electron transport in the solar atmosphere. By building on previous results, this treatment does not require explici...

The phase function for stellar acoustic oscillations - IV . Solar - like stars

In recent years there has been some progress towards detecting solar-like oscillations in stars. The goal of this challenging project is to analyse frequency spectra similar to that observed for the Sun in integrated light. In this context it is important to investigate what can be learned about the structure and evolution of the stars from such future observations. Here we concentrate on the s...