The Sun as an X-Ray Star. II. Using the Yohkoh/Soft X-Ray Telescope-derived Solar Emission Measure versus Temperature to Interpret Stellar X-Ray Observations

By Giovanni Peres, S. Orlando, Fabio Reale, R. Rosner, H. Hudson. 2000

166 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/99203ab9d641ca9230538b430447ca781d82972c

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In Astronomy and Astrophysics

Citations in the corpus

Simulations of the Photospheric Magnetic Activity and Outer Atmospheric Radiative Losses of Cool Stars Based on Characteristics of the Solar Magnetic Field (2001, background): “This is indeed observed for the Sun (Peres et al. 2000).”
X-Ray-emitting Young Stars in the Orion Nebula (2002, background): “Integrated over its disk and viewed with CCD spectral resolution, the Sun typically would be seen at a plasma energy 0.2 keV, rising to 0.6 keV during powerful flares (Peres et al. 2000; Reale, Peres, & Orlando 2001).”
The Extreme Ultraviolet and X-Ray Sun in Time: High-Energy Evolutionary Tracks of a Solar-Like Star (2015, unknown): “The solarLX (6×1026− 5× 1027 erg s−1, Ayres (1997); Peres et al. (2000); Judge et al. (2003)”
THE STELLAR-ACTIVITY–ROTATION RELATIONSHIP AND THE EVOLUTION OF STELLAR DYNAMOS (2011, background): “This slope also produces a much better fit to the Sun’s RX , over-predicting it’s luminosity by only 0.2 dex.”
Stellar magnetism: empirical trends with age and rotation (2014, background): “For the Sun, it is observed that during its activity cycle, the X-ray luminosity varies from ' 0.27 to 4.7×1027 erg s−1 at minimum and maximum phases, respectively (Peres et al. 2000).”
Coronal Loops: Observations and Modeling of Confined Plasma (2010, background): “It was applied to flares (Reale et al., 2001) and to describe the evolution of active regions (Orlando et al.”
X-rays from solar system objects (2007, background): “X-ray photon among 5×10 11 photons from Venus. The extremely low ratio between the X-ray and optical flux from Venus is mainly caused by the comparatively low X-ray luminosity of the Sun (~4×10 20 W; Peres et al., 2000) and the small fluorescence yields of light elements (0.25% for C and 0.85% for O”
Magnetic Flaring in the Pre-Main-Sequence Sun and Implications for the Early Solar System (2002, background): “For comparison, in the same band the contemporary Sun emits typically logLX ’ 25:3 ergs s 1 with T ’ 1 MK during its quiet phase, logLX ’ 27:0 ergs s 1 during maximum phase with T ’ 2 5 MK, and around logLX ’ 28:0 ergs s 1 with T ’ 2 20 MK during a powerful (1992 November 2) flare (Peres et al. 2000”
The Sun in Time: Activity and Environment (2007, background): “Peres et al. (2000) have studied the fulldisk solar coronal emission measure distribution to find peak temperatures of ≈ 1 MK and ≈ 2 MK during minimum and maximum, respectively.”
Heating and Ionization of X-Winds (2001, methodology): “The simulations of the Sun as an X-ray star (Peres et al. 2000), based on modeling of Yohkoh Soft X-Ray Telescope observations, suggest that the high-energy component seen in low-resolution astronomical satellite measurements of YSOs is associated with small and large Ñares.”