Synoptic maps for the heliospheric Thomson scattering brightness as observed by the HELIOS photometers

Details Synoptic maps for the heliospheric Thomson scattering brightness as observed by the HELIOS photometers Synoptic maps for the heliospheric Thomson scattering brightness as observed by the HELIOS photometers

Apr 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...244..242h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 244, no. 1, April 1991, p. 242-250.

Astronomy and Astrophysics

Astrophysics

2

Astronomical Photometry, Helios Satellites, Heliosphere, Solar Corona, Thomson Scattering, Brightness Distribution, Magnetic Field Configurations, Solar Magnetic Field, Synoptic Measurement

Scientific paper

A method for displaying the electron Thomson scattering intensity in the inner heliosphere as observed by the zodiacal light photometers on board the Helios spacecraft in the form of synoptic maps is presented. The method is based on the assumption that the bulk of the scattering electrons along the line of sight is located near the point closest to the sun. Inner-heliospheric structures will generally be represented properly in these synoptic maps only if they are sufficiently long-lived (that is, a significant fraction of a solar rotation period). The examples of Helios synoptic maps discussed (from data in April 1976 and November 1978), indicate that it is possible to identify large-scale, long-lived density enhancements in the inner heliosphere. It is expected that the Helios synoptic maps will be particularly useful in the study of corotating structures (e.g., streamers), and the maps will be most reliable during periods when few transient featurs are present in the corona, i.e., during solar minimum.

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