• Publications
  • Influence
The Sun as an X-Ray Star. II. Using theYohkoh/Soft X-Ray Telescope-derived Solar Emission Measure versus Temperature to Interpret Stellar X-Ray Observations
This paper is the second of a project dedicated to using solar Yohkoh/SXT data as a guide and a template to interpret data on stellar coronae. In the light of the large diUerences in scope and
Bright X-Ray Flares in Orion Young Stars from COUP: Evidence for Star-Disk Magnetic Fields?
We have analyzed a number of intense X-ray flares observed in the Chandra Orion Ultradeep Project (COUP), a 13 day observation of the Orion Nebula Cluster (ONC), concentrating on the events with the
Diagnostics of stellar flares from X-ray observations: from the decay to the rise phase
Context. The diagnostics of stellar flaring coronal loops have been so far largely based on the analysis of the decay phase. Aims. We derive new diagnostics from the analysis of the rise and peak
Flares from small to large: X-ray spectroscopy of Proxima Centauri with XMM-Newton
We report results from a comprehensive study of the nearby M dwarf Proxima Centauri with the XMM-Newton satellite, using simultaneously its X-ray detectors and the Optical Monitor with its U band
XMM-Newton observations of the supernova remnant IC 443: II. evidence of stellar ejecta in the inner regions.
Aims. We investigate the spatial distribution of the physical and chemical properties of the hot X-ray emitting plasma of the supernova remnant IC 443, in order to get important constraints on its
Coronal Loops: Observations and Modeling of Confined Plasma
  • F. Reale
  • Physics
    Living reviews in solar physics
  • 28 October 2010
This review focuses on coronal loops mostly as structures confining plasma, and topics such as loop oscillations and flaring loops (except for non-solar ones which provide information on stellar loops) are not specifically addressed here.
Crushing of interstellar gas clouds in supernova remnants. I. The role of thermal conduction and radiative losses
We model the hydrodynamic interaction of a shock wave of an evolved supernova remnant with a small interstellar gas cloud like the ones observed in the Cygnus loop and in the Vela SNR. We investigate
On the origin of asymmetries in bilateral supernova remnants
Aims. We investigate whether the morphology of bilateral supernova remnants (BSNRs) observed in the radio band is determined mainly either by a non-uniform interstellar medium (ISM) or by a
Evidence of nonthermal particles in coronal loops heated impulsively by nanoflares
This analysis provides tight constraints on the properties of electron beams and new diagnostics for their presence in the nonflaring corona through high-resolution observations with the IRIS.
On the observability of T Tauri accretion shocks in the X-ray band
Context. High resolution X-ray observations of classical T Tauri stars (CTTSs) show a soft X-ray excess due to high density plasma (ne = 10 11 −10 13 cm −3 ). This emission has been attributed to