scholarly journals A Search for Small Scale Structures in the Zodiacal Light

1985 ◽  
Vol 85 ◽  
pp. 33-37
Author(s):  
S.S. Hong ◽  
N.Y. Misconi ◽  
M.H.H. van Dijk ◽  
J.L. Weinberg ◽  
G.N. Toller
Keyword(s):  
Brightness Distribution ◽  
Empirical Method ◽  
Asteroid Belt ◽  
Small Scale ◽  
High Angular Resolution ◽  
Zodiacal Light ◽  
Radiation Background ◽  
Scale Structures ◽  
Pioneer 10 ◽  
Small Scale Structures

AbstractGegenschein observations from Pioneer 10 were found to have brightness structures with an amplitude of about 10% and a period of several to ten degrees in elongation. A search is made for such structures in high angular resolution ground-based observations from Mt. Haleakala, Hawaii. A new empirical method is used to correct for atmosphere-originated radiation. Background starlight is subtracted using Pioneer 10 observations from beyond the asteroid belt. Preliminary analysis of the ground data also indicates the presence of small amplitude structures in the brightness distribution.

A Search for Small Scale Structures in the Zodiacal Light

1985 ◽  
pp. 33-37 ◽  
Author(s):  
S. S. Hong ◽  
N. Y. Misconi ◽  
M. H. H. van Dijk ◽  
J. L. Weinberg ◽  
G. N. Toller
Keyword(s):  
Small Scale ◽  
Zodiacal Light ◽  
Scale Structures ◽  
Small Scale Structures

Exploring Coronal Structures with SOHO

2000 ◽  
Vol 179 ◽  
pp. 403-406
Author(s):  
M. Karovska ◽  
B. Wood ◽  
J. Chen ◽  
J. Cook ◽  
R. Howard
Keyword(s):  
Solar Corona ◽  
Image Enhancement ◽  
Coronal Mass Ejections ◽  
Dynamical Evolution ◽  
Small Scale ◽  
Low Contrast ◽  
Contrast Structures ◽  
Scale Structures ◽  
Small Scale Structures ◽  
Coronal Structures

AbstractWe applied advanced image enhancement techniques to explore in detail the characteristics of the small-scale structures and/or the low contrast structures in several Coronal Mass Ejections (CMEs) observed by SOHO. We highlight here the results from our studies of the morphology and dynamical evolution of CME structures in the solar corona using two instruments on board SOHO: LASCO and EIT.

scholarly journals Observational aspects of prominence oscillations

2007 ◽  
Vol 3 (S247) ◽  
pp. 152-157 ◽  
Author(s):  
Oddbjørn Engvold
Keyword(s):  
Magnetic Structure ◽  
Numerical Models ◽  
Small Scale ◽  
Solar Prominences ◽  
Scale Structures ◽  
Oscillations And Waves ◽  
Available Information ◽  
Small Scale Structures

AbstractSeismology has become a powerful tool in studies of the magnetic structure of solar prominences and filaments. Reversely, analytical and numerical models are guided by available information about the spatial and thermodynamical structure of these enigmatic structures. The present invited paper reviews recent observational results on oscillations and waves as well as details about small-scale structures and dynamics of prominences and filaments.

scholarly journals Detailed maps of interstellar clouds in front of ω Centauri: small-scale structures in the Galactic disc-halo interface

2009 ◽  
Vol 399 (1) ◽  
pp. 195-208 ◽  
Author(s):  
Jacco Th. van Loon ◽  
Keith T. Smith ◽  
Iain McDonald ◽  
Peter J. Sarre ◽  
Stephen J. Fossey ◽  
...  
Keyword(s):  
Small Scale ◽  
Galactic Disc ◽  
Interstellar Clouds ◽  
Scale Structures ◽  
Small Scale Structures

scholarly journals Stationary magnetospheric convection on November 24, 1981. 2. Small-scale structures in the dayside cusp/cleft

1999 ◽  
Vol 17 (3) ◽  
pp. 375 ◽  
Author(s):  
Y. I. Galperin ◽  
J. M. Bosqued ◽  
R. A. Kovrazhkin ◽  
A. G. Yahnin
Keyword(s):  
Small Scale ◽  
Magnetospheric Convection ◽  
Scale Structures ◽  
Small Scale Structures

scholarly journals GAMMA RAYS FROM SMALL SCALE STRUCTURES ON LONG COSMIC STRINGS

1993 ◽  
Vol 02 (02) ◽  
pp. 183-195 ◽  
Author(s):  
M. MOHAZZAB ◽  
R. BRANDENBERGER
Keyword(s):  
Gamma Rays ◽  
Gamma Ray ◽  
Cosmic Strings ◽  
Unit Length ◽  
Formation Rate ◽  
Long Strings ◽  
Small Scale ◽  
Scale Structures ◽  
Cusp Formation ◽  
Small Scale Structures

The formation of cusps on long cosmic strings is discussed and the probability of cusp formation is estimated. The energy distribution of the gamma-ray background due to cusp annihilation on long strings is calculated and compared to observations. Under optimistic assumptions about the cusp formation rate, we find that strings with a mass per unit length μ less than Gμ=10−14 will have an observable effect. However, it is shown that the gamma-ray bursters cannot be attributed to long ordinary strings (or loops).

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