Constraining the CME Core Heating and Energy Budget with SOHO/UVCS

  title={Constraining the CME Core Heating and Energy Budget with SOHO/UVCS},
  author={Maurice L. Wilson and John C. Raymond and Susan T. Lepri and Roberto Lionello and Nicholas A. Murphy and Katharine K. Reeves and Chengcai Shen},
  journal={The Astrophysical Journal},
We describe the energy budget of a coronal mass ejection (CME) observed on 1999 May 17 with the Ultraviolet Coronagraph Spectrometer (UVCS). We constrain the physical properties of the CME’s core material as a function of height along the corona by using the spectra taken by the single-slit coronagraph spectrometer at heliocentric distances of 2.6 and 3.1 solar radii. We use plasma diagnostics from intensity ratios, such as the O vi doublet lines, to determine the velocity, density, temperature… 
1 Citations
On Modeling ICME Cross-Sections as Static MHD Columns
Solar coronal mass ejections are well known to expand as they propagate through the heliosphere. Despite this, their cross-sections are usually modeled as static plasma columns within the


SOHO Observations of a Coronal Mass Ejection
We describe a coronal mass ejection (CME) observed on 1999 April 23 by the Ultraviolet Coronagraph Spectrometer (UVCS), the Extreme-Ultraviolet Imaging Telescope (EIT), and the Large-Angle and
Efficiency variations of UVCS/SOHO based on laboratory measurements of replica gratings
We have carried out measurements of efficiency as functions of position across the surfaces of replica grating made from the same masters as the UVCS/SOHO flight units. Variations in first order
Stray light, radiometric, and spectral characterization of UVCS/SOHO: laboratory calibration and flight performance
The Ultraviolet Coronagraph Spectrometer is one of the instruments on board the Solar and Heliospheric Observatory spacecraft, which was launched in December, 1995. The instrument is designed to make
A Lagrangian scheme for time-dependent ionization in simulations of astrophysical plasmas
On 1999 August 26, a coronal jet occurred at the northwest limb near a sigmoid active region (AR 8668) that was the target for a joint observation plan (SOHO joint observing program 106) during the
Ultraviolet spectroscopy of the extended solar corona
The first observations of ultraviolet spectral line profiles and intensities from the extended solar corona (i.e., more than 1.5 solar radii from Sun-center) were obtained on 13 April 1979 when a
On the Radial and Longitudinal Variation of a Magnetic Cloud: ACE, Wind, ARTEMIS and Juno Observations
We present observations of the same magnetic cloud made near Earth by the Advance Composition Explorer (ACE), Wind, and the Acceleration, Reconnection, Turbulence and Electrodynamics of the Moon’s
The Effect of Solar Wind Expansion and Nonequilibrium Ionization on the Broadening of Coronal Emission Lines
When observing spectral lines in the optically-thin corona, line-of-sight (LOS) effects can strongly affect the interpretation of the data, especially in regions just above the limb. We present a
CME–CME Interactions as Sources of CME Geoeffectiveness: The Formation of the Complex Ejecta and Intense Geomagnetic Storm in 2017 Early September
Coronal mass ejections (CMEs) are the primary sources of intense disturbances at Earth, where their geo-effectiveness is largely determined by their dynamic pressure and internal magnetic field,