Chandra Observation of the ρ Ophiuchi Cloud

By K. Imanishi, K. Koyama, Y. Tsuboi. 2001

172 citations recorded by the source corpus.

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In Astronomy and Astrophysics

Citations in the corpus

Solar Flares: Magnetohydrodynamic Processes (2011, background): “, 1998; Imanishi et al., 2001, see Feigelson and Montmerle, 1999 for a review). Time variation of X-ray intensity is similar to that of solar flares, while the total energy released by those stellar flares amounts to 10(36) – 10(37) erg, much larger than those of solar flares. Can these protostellar”
X-Ray-emitting Young Stars in the Orion Nebula (2002, background): “By a considerable factor, this is the largest sample of X-ray detected PMS VLM objects yet obtained; previously samples are reported by Neuhäuser et al. (1999), Imanishi et al. (2001), and Preibisch & Zinnecker (2001).”
Accretion in the ρ-Ophiuchi pre-main sequence stars (2006, methodology): “X-ray observations of Ophiuchus have been recently carried out with Chandra and XMM satellites by Imanishi et al. (2001) and Ozawa et al. (2005).”
EXCLUSION OF COSMIC RAYS IN PROTOPLANETARY DISKS: STELLAR AND MAGNETIC EFFECTS (2013, background): “…has been observed that objects with high stellar X-ray luminosity (LXR & 1031 erg s−1) typically have harder X-ray spectra at energies exceeding 2 keV, characteristic of emission contribution from stellar flares (Carkner et al. 1996; Imanishi et al. 2001; Wolk et al. 2005; Preibisch et al. 2005).”
Determination of the gas-to-dust ratio in nearby dense clouds using X-ray absorption measurements (2003, background): “In the core B and F region, Imanishi et al. (2001a) identified 58 X-ray sources with near-IR counterparts.”
The Sun in Time: Activity and Environment (2007, background): “Such relations continue to hold into the PMS domain where exceedingly hot coronae with temperatures up to ≈ 100 MK are found (Imanishi et al., 2001).”
X-ray spectroscopy of stars (2009, methodology): “Flaring is common in TTS (Stelzer et al, 2007), the most energetic examples reaching temperatures of≈ 108 K (Imanishi et al, 2001).”
Magnetic Flaring in the Pre-Main-Sequence Sun and Implications for the Early Solar System (2002, background): “Imanishi et al. (2001) report that the emitting and reflecting components in YLW 16A vary together with a delay shorter than 104 lt-s, indicating that the flare-disk distance is less than 15 AU.”
Protoplanetary disc evolution and dispersal: the implications of X-ray photoevaporation (2010, background): “Therefore, due to their higher X-ray temperature flares tend to emit most of their radiation in the hard X-ray region (as shown by observations of objects in a ‘flare’ state compared to in a ‘quiescent’ state, e.g. Imanishi et al. 2001), where the thermal impact is low, as discussed above.”
Bolocam Survey for 1.1 mm Dust Continuum Emission in the c2d Legacy Clouds. I. Perseus (2005, background): “The cluster region has been studied in great detail at a variety of wavelengths from millimeter molecular lines (Loren 1989; Ridge et al. 2006) to near-infrared (e.g., Wilking et al. 1989; Allen et al. 2002) to X-ray (Imanishi et al. 2001).”