scholarly journals Observation of a large amplitude wave and inversion layer leading to convective instability in the mesopause region over Fort Collins, CO (41°N, 105°W)

2002 ◽  
Vol 29 (17) ◽  
pp. 31-1-31-4 ◽  
Author(s):  
Bifford P. Williams ◽  
M. A. White ◽  
D. A. Krueger ◽  
C. Y. She
Keyword(s):  
Large Amplitude ◽  
Convective Instability ◽  
Inversion Layer ◽  
Amplitude Wave ◽  
Mesopause Region ◽  
Fort Collins ◽  
And Inversion ◽  
Large Amplitude Wave

scholarly journals Strong Waves from Pulsars and Morphologies in SNRs

1983 ◽  
Vol 101 ◽  
pp. 499-501
Author(s):  
Gregory Benford ◽  
Attilio Ferrari ◽  
Silvano Massaglia
Keyword(s):  
Large Amplitude ◽  
Crab Nebula ◽  
Surrounding Medium ◽  
Low Frequency ◽  
Optical Emission ◽  
Amplitude Wave ◽  
Surface Magnetic Field ◽  
Plasma Absorption ◽  
The Crab Nebula ◽  
Large Amplitude Wave

Canonical models for pulsars predict the emission of low–frequency waves of large amplitudes, produced by the rotation of a neutron star possessing a strong surface magnetic field. Pacini (1968) proposed this as the basic drain which yields to the pulsar slowing–down rate. The main relevance of the large amplitude wave (LAW) is the energetic link it provides between the pulsar and the surrounding medium. This role has been differently emphasized (Rees and Gunn, 1974; Ferrari, 1974), referring to absorption effects by relativistic particle acceleration and thermal heating, either close to the pulsar magnetosphere or in the nebula. It has been analyzed in the special case of the Crab Nebula, where observations are especially rich (Rees, 1971). As the Crab Nebula displays a cavity around the pulsar of dimension ∼1017cm, the function of the wave in sweeping dense gas away from the circumpulsar region is widely accepted. Absorption probably occurs at the inner edges of the nebula; i.e., where the wave pressure and the nebular pressure come into balance. Ferrari (1974) interpreted the wisps of the Crab Nebula as the region where plasma absorption occurs, damping the large amplitude wave and driving “parametric” plasma turbulence, thus trasferring energy to optical radiation powering the nebula. The mechanism has been extended to interpret the specific features of the “wisps” emission (Benford et al., 1978). Possibly the wave fills the nebula completely, permeating the space outside filaments with electromagnetic energy, continuously accelerating electrons for the extended radio and optical emission (Rees, 1971).

Enhancement of damping of a large amplitude wave

1975 ◽  
Vol 18 (1) ◽  
pp. 114 ◽  
Author(s):  
Ryo Sugihara ◽  
Kaoru Yamanaka
Keyword(s):  
Large Amplitude ◽  
Amplitude Wave ◽  
Large Amplitude Wave

An Optlcal and Radio Investigation of the Active RS CVn Star HD 127535

1985 ◽  
Vol 6 (2) ◽  
pp. 160-164 ◽  
Author(s):  
J. L. Innis ◽  
D. W. Coates ◽  
K. Thompson ◽  
G. J. Nelson ◽  
O. B. Slee ◽  
...  
Keyword(s):  
Radio Emission ◽  
Time Scales ◽  
Radio Telescope ◽  
Large Amplitude ◽  
Amplitude Wave ◽  
Preliminary Results ◽  
Photometric Measurements ◽  
5 Ghz ◽  
Large Amplitude Wave ◽  
Photometric Variation

AbstractWe present some preliminary results of an optical and radio study of the very active RS CVn binary HD 127535. Photometric measurements show the presence of a large amplitude wave which exhibits marked changes in shape and range on time scales as short as a few months. This photometric variation is almost certainly due to large cool starspots on the cooler, more luminous component. As part of a survey of southern active-chromosphere stars with the Parkes radio telescope, HD 127535 has been observed at 5, 8.4 and 22 GHz. No detection was made at 5 GHz, possibly because of confusion due to the angular proximity of the star to the galatic plane. However, it is one of the strongest sources detected in the 8.4 GHz survey, and is one of only two stars detected at 22 GHz. Photometry obtained two cycles before the 8.4 GHz observations suggest a possible correlation between the radio emission and the photometric wave, i.e. spot visibility, but more data are needed.

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