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Wepresentthefirstquantitativecomparisonbetweenthetotalmagneticreconnectionfluxinthelowcoronainthe wake of coronal mass ejections (CMEs) and the magnetic flux in magnetic clouds (MCs) that reach 1 AUExpand
Earthshine observations of the Earth's reflectance
Regular photometric observations of the moon's “ashen light” (earthshine) from the Big Bear Solar Observatory (BBSO) since December 1998 have quantified the earth's optical reflectance. We find largeExpand
Magnetic reconnection flux and coronal mass ejection velocity
We explore the relationship between the total reconnection flux ψrec estimated from flare observations and the velocity VCME of coronal mass ejections (CMEs) observed with the Large Angle andExpand
Near-Infrared Observations at 1.56 Microns of the 2003 October 29 X10 White-Light Flare
We present high-resolution observations of an X10 white-light flare in solar NOAA Active Region 10486 obtained with the Dunn Solar Telescope (DST) at the National Solar Observatory/Sacramento Peak onExpand
Ultraviolet and Hα Emission in Ellerman Bombs
We present the first high-cadence time profiles of Ellerman bombs (EBs) at two wavelengths, 1.3 A in the blue wing of the Hα line and the UV continuum at 1600 A, and study their temporal correlation.Expand
Extreme-ultraviolet jets and hα surges in solar microflares
We analyzed simultaneous EUV data from the Transition Region and Coronal Explorer and Hα data from Big Bear Solar Observatory. In the active region studied, we found several EUV jets that repeatedlyExpand
Modeling and Measuring the Flux Reconnected and Ejected by the Two-Ribbon Flare/CME Event on 7 November 2004
Abstract Observations of the large two-ribbon flare on 7 November 2004 made using SOHO and TRACE data are interpreted in terms of a three-dimensional magnetic field model. Photospheric flux evolutionExpand
The Formation of a Prominence in Active Region NOAA 8668. I. SOHO/MDI Observations of Magnetic Field Evolution
We have studied the evolution of the photospheric magnetic —eld in active region NOAA 8668 for 3 days while the formation of a reverse S-shaped —lament proceeded. From a set of full-diskExpand
Earthshine and the Earth's albedo: 2. Observations and simulations over 3 years
[1] Since late 1998, we have been making sustained measurements of the Earth's reflectance by observing the earthshine from Big Bear Solar Observatory. Further, we have simulated the Earth'sExpand
IRIS observations of the Mg ii h and k lines during a solar flare
The bulk of the radiative output of a solar flare is emitted from the chromosphere, which produces enhancements in the optical and UV continuum, and in many lines, both optically thick and thin. WeExpand