The bulk of X-ray emission from pre-main-sequence (PMS) stars is coronal in origin. We demonstrate herein that stars on Henyey tracks in the Hertzsprung-Russell diagram have lower log(LX/L*), on average, than stars on Hayashi tracks. This effect is driven by the decay of LX once stars develop radiative cores. LX decays faster with age for intermediate mass PMS stars, the progenitors of main sequence A-type stars, compared to those of lower mass. As almost all main sequence A-type stars show no detectable X-ray emission, we may already be observing the loss of their coronae during their PMS evolution. Although there is no direct link between the size or mass of the radiative core and LX, the longer stars have spent with partially convecti...
In Chapter I, I introduce the framework of observational and theoretical evidence that has been cons...
Solar-type stars exhibit their highest levels of magnetic activity during early convective pre-main ...
Measuring the evolution of X-ray emission from pre-main sequence (PMS) stars gives insight into two ...
The bulk of X-ray emission from pre-main-sequence (PMS) stars is coronal in origin. We demonstrate h...
Pre-main-sequence (PMS) stars of mass ≳0.35 M☉ transition from hosting fully convective interiors to...
SGG acknowledges support from the Science & Technology Facilities Council (STFC) via an Ernest Ruthe...
Measuring the evolution of X-ray emission from pre-main sequence (PMS) stars gives insight into two ...
Context. The first million years of the pre-main-sequence (PMS) evolution of low-mass stars are char...
We investigate the evolution of X-ray stellar activity from the age of the youngest known star formi...
International audienceThe angular momentum evolution of cool stars during the pre-main sequence phas...
The large-scale magnetic fields of several pre-main sequence (PMS) stars have been observed to be si...
Aims. We study the X-ray emission of low-mass main-sequence stars to derive a reliable gen...
We present a comprehensive picture of the relative emission and heating of the chromospheres and cor...
We present the Pre-Main Sequence (PMS) evolutionary tracks of stars with 0.065~5.0M_⨀. The models we...
In Chapter I, I introduce the framework of observational and theoretical evidence that has been cons...
Solar-type stars exhibit their highest levels of magnetic activity during early convective pre-main ...
Measuring the evolution of X-ray emission from pre-main sequence (PMS) stars gives insight into two ...
The bulk of X-ray emission from pre-main-sequence (PMS) stars is coronal in origin. We demonstrate h...
Pre-main-sequence (PMS) stars of mass ≳0.35 M☉ transition from hosting fully convective interiors to...
SGG acknowledges support from the Science & Technology Facilities Council (STFC) via an Ernest Ruthe...
Measuring the evolution of X-ray emission from pre-main sequence (PMS) stars gives insight into two ...
Context. The first million years of the pre-main-sequence (PMS) evolution of low-mass stars are char...
We investigate the evolution of X-ray stellar activity from the age of the youngest known star formi...
International audienceThe angular momentum evolution of cool stars during the pre-main sequence phas...
The large-scale magnetic fields of several pre-main sequence (PMS) stars have been observed to be si...
Aims. We study the X-ray emission of low-mass main-sequence stars to derive a reliable gen...
We present a comprehensive picture of the relative emission and heating of the chromospheres and cor...
We present the Pre-Main Sequence (PMS) evolutionary tracks of stars with 0.065~5.0M_⨀. The models we...
In Chapter I, I introduce the framework of observational and theoretical evidence that has been cons...
Solar-type stars exhibit their highest levels of magnetic activity during early convective pre-main ...
Measuring the evolution of X-ray emission from pre-main sequence (PMS) stars gives insight into two ...