TY - JOUR

T1 - Solar brightness distribution and its variability at 3 millimeter wavelength

AU - Nagnibeda, V. G.

AU - Piotrovitch, V. V.

PY - 1994/6/1

Y1 - 1994/6/1

N2 - Solar mapping at 3.4 millimeter wavelength has shown the existence of various spatial structures in brightness distribution. The most prominent structure is presented by the local sources of the slowly varying component of the solar radio emission. Usually they coincide with active regions. Some sources have no corresponding optical counterparts. Using synoptic radio maps, latitudinal belts of enhanced brightness were detected at the north and south hemispheres. These belts seem to coincide with sunspot zones, but the enhanced emission exists independently of sunspot group appearance. Comparison of our maps with XUV images shows a noticeable resemblance. Sources above active regions and latitudinal belts of enhanced brightness are seen in both ranges as well as coronal holes.

AB - Solar mapping at 3.4 millimeter wavelength has shown the existence of various spatial structures in brightness distribution. The most prominent structure is presented by the local sources of the slowly varying component of the solar radio emission. Usually they coincide with active regions. Some sources have no corresponding optical counterparts. Using synoptic radio maps, latitudinal belts of enhanced brightness were detected at the north and south hemispheres. These belts seem to coincide with sunspot zones, but the enhanced emission exists independently of sunspot group appearance. Comparison of our maps with XUV images shows a noticeable resemblance. Sources above active regions and latitudinal belts of enhanced brightness are seen in both ranges as well as coronal holes.

UR - http://www.scopus.com/inward/record.url?scp=5244312023&partnerID=8YFLogxK

U2 - 10.1007/BF01473201

DO - 10.1007/BF01473201

M3 - Article

AN - SCOPUS:5244312023

VL - 152

SP - 175

EP - 180

JO - Solar Physics

JF - Solar Physics

SN - 0038-0938

IS - 1

ER -