Stephen M. White

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We present here the rst images of impulsive millimeter emission of a are. The are on 1994 August 18 was simultaneously observed at millimeter (86 GHz), microwave (1-18 GHz), and soft and hard X{ray wavelengths. Images of millimeter, soft and hard X{ray emission show the same compact (< 8 00) source. Both the impulsive and the gradual phases are studied in(More)
The relationship of our emotions and psyche to heart disease is intriguing. In this article we have reviewed the evidence linking cardiovascular and neuropsychiatric disorders and the possible mechanisms and pathophysiology of this association. This review is derived from Medline searches (1966-2002) using the relevant search terms (psychiatric disease,(More)
A radio frequency interference (RFI) excision algorithm based on spectral domain statistics is proposed and implemented in software. The algorithm requires the use of two memory buffers, S 1 and S 2 , in which the first two powers of M power spectral density (PSD) estimates, obtained via Fast Fourier Transform (FFT), are accumulated and used to form a(More)
The temporal relationship between coronal mass ejections (CMEs) and associated solar Ñares is of great importance to understanding the origin of CMEs, but it has been difficult to study owing to the nature of CME detection. In this paper, we investigate this issue using the Large Angle and Spectro-metric Coronagraph and the EUV Imaging Telescope(More)
—This paper deals with a feasibility study for a System-on-Chip (SoC) mm-wave radiometer devoted to space-based observation of solar flares and operating in the Ka-band. The radiometer has been designed in 250 nm SiGe BiCMOS process. The circuit integrates a three stages differential LNA with 37.2 dB gain and 4.8 dB noise figure at 36.8 GHz and a(More)
We present a detailed examination on the nonthermal emissions during the preflare phase of the X4.8 flare that occurred on 2002 July 23. The microwave (17 GHz and 34 GHz) data obtained with Nobeyama Radioheliograph, at Nobeyama Solar Radio Observatory and the hard X-ray data taken with Reuven Ramaty High Energy Solar Spectroscopic Imager obviously showed(More)
Determining the 3D coronal magnetic field is a critical, but extremely difficult problem to solve. Since different types of multiwavelength coronal data probe different aspects of the coronal magnetic field, ideally these data should be used together to validate and constrain specifications of that field. Such a task requires the ability to create(More)
The measurement of magnetic field strengths in the solar corona using radio observations is reviewed. This is a well established technique that exploits the fact that the electron gyrofrequency for typical coronal magnetic field strengths (100–2000 Gauss) lies in the radio frequency range. Opacity from the resulting gyroresonance emission from hot plasma(More)