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Space Science Reviews, 1964
This paper is a review of our observational knowledge on solar magnetic fields. In Section 1 we make an attempt to summarize all observations of the general magnetic field (m.f.) of the Sun. Section 2 deals with the local m.f. at low latitudes and their connection with some features on the disk. The m.f.
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This paper is a review of our observational knowledge on solar magnetic fields. In Section 1 we make an attempt to summarize all observations of the general magnetic field (m.f.) of the Sun. Section 2 deals with the local m.f. at low latitudes and their connection with some features on the disk. The m.f.
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Geomagnetism and Aeronomy, 2013
The solar polar magnetic field has attracted the attention of researchers since the polar magnetic field reversal was revealed in the middle of the last century (Babcock and Livingston, 1958). The polar magnetic field has regularly reversed because the magnetic flux is transported from the sunspot formation zone owing to differential rotation ...
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The solar polar magnetic field has attracted the attention of researchers since the polar magnetic field reversal was revealed in the middle of the last century (Babcock and Livingston, 1958). The polar magnetic field has regularly reversed because the magnetic flux is transported from the sunspot formation zone owing to differential rotation ...
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1977
Abstract : This report describes a series of observations of solar magnetic fields. These observations were made using narrow band filters and active seeing correction systems developed at the Lockheed Palo Alto Research Laboratories. New data has been obtained concerning the strength and size of solar magnetic field elements, and which set an upper ...
Alan M. Title, Robert C. Smithson
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Abstract : This report describes a series of observations of solar magnetic fields. These observations were made using narrow band filters and active seeing correction systems developed at the Lockheed Palo Alto Research Laboratories. New data has been obtained concerning the strength and size of solar magnetic field elements, and which set an upper ...
Alan M. Title, Robert C. Smithson
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1966
Abstract : A study was conducted of the correspondence of photospheric magnetic fields with structures and transient phenomena observed in the chromosphere. The primary data used were isogauss maps constructed from the Mt. Wilson daily, full disk magnetograms for the period 1959 through 1962, and three fine-scan magnetograms made on 6 July 1965.
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Abstract : A study was conducted of the correspondence of photospheric magnetic fields with structures and transient phenomena observed in the chromosphere. The primary data used were isogauss maps constructed from the Mt. Wilson daily, full disk magnetograms for the period 1959 through 1962, and three fine-scan magnetograms made on 6 July 1965.
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Solar Magnetic Fields - Extended
Publications of the Astronomical Society of the Pacific, 1971Spacecraft observations of the interplanetary magnetic field have revealed that almost always each solar rotation can be divided into sectors, within each of which the field has a predominant polarity toward the sun or away from the sun. Comparisons of this interplanetary magnetic sector pattern with observations of the photospheric magnetic field have
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2003
The proximity of the Sun allows us to make detailed measurements on the properties of solar magnetic fields. The long term systematic changes in the solar magnetic field pattern indicate a global origin. A global dynamo can be sustained by the interaction of solar convection with solar rotation.
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The proximity of the Sun allows us to make detailed measurements on the properties of solar magnetic fields. The long term systematic changes in the solar magnetic field pattern indicate a global origin. A global dynamo can be sustained by the interaction of solar convection with solar rotation.
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AIP Conference Proceedings, 1992
Intrinsically weak magnetic fields are difficult to identify, since flux measurements (magnetograms) cannot by themselves distinguish between filling‐factor and field‐strength effects. The first real determinations of intrinsically weak (less than kG) fields have in fact been made only this year, using the Stokes V profiles of an infrared line pair ...
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Intrinsically weak magnetic fields are difficult to identify, since flux measurements (magnetograms) cannot by themselves distinguish between filling‐factor and field‐strength effects. The first real determinations of intrinsically weak (less than kG) fields have in fact been made only this year, using the Stokes V profiles of an infrared line pair ...
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1985
1 Introduction to Solar Activity.- 1.1 Some Basic Properties of the Sun.- 1.2 Basic Equations of Magnetohydrodynamic.- 1.2.1 Magnetohydrostatics.- 1.2.2 Waves.- 1.2.3 Instabilities.- 1.3 Sunspots.- 1.4 Prominences.- 1.4.1 Prominence Formation.- 1.4.2 Magnetostatic Support.- 1.5 The Corona.- 1.5.1 Models of the Corona.- 1.5.2 Coronal Heating.- 1.6 Solar
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1 Introduction to Solar Activity.- 1.1 Some Basic Properties of the Sun.- 1.2 Basic Equations of Magnetohydrodynamic.- 1.2.1 Magnetohydrostatics.- 1.2.2 Waves.- 1.2.3 Instabilities.- 1.3 Sunspots.- 1.4 Prominences.- 1.4.1 Prominence Formation.- 1.4.2 Magnetostatic Support.- 1.5 The Corona.- 1.5.1 Models of the Corona.- 1.5.2 Coronal Heating.- 1.6 Solar
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Solar Magnetic Fields and Convection
Astrophysics and Space Science, 1976We review the primordial field theory of solar magnetic fields (Papers I–VI) whose three main features are, first, a permanent dipole-like magnetic field, second a mainly toroidal field formed by shearing and rolling into individual, helically twisted ropes as suggested by Babcock, and third a mechanism for reversing the toroidal field.
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