Results 211 to 220 of about 14,143 (259)

Day-to-Day Boundary Fluctuations in Coronal Holes: Causes and Consequences. [PDF]

Sol Phys
Ugarte-Urra I, Wang YM, Muglach K, Sheeley NR.   +3 more
europepmc   +1 more source

Synergetic properties of advanced materials for high-power and high-temperature applications. [PDF]

Discov Nano
Mengesha WG, Nagessar K.
europepmc   +1 more source

IMAP's Role in Understanding Particle Injection and Energization Throughout the Heliosphere. [PDF]

Space Sci Rev
Cohen CMS, Alterman BL, Baker DN, Bruno A, Bzowski M, Christian ER, Cohen IJ, Dalla S, Dayeh MA, Desai MI, Elliott HA, Giacalone J, Gkioulidou M, Guo F, Horbury T, Kanekal SG, Kowalska-Leszczyńska I, Lee CO, Livadiotis GI, Luhmann JG, Matthaeus WH, McComas DJ, Mitchell JG, Moebius E, Rankin J, Richardson JD, Schwadron NA, Skoug R, Turner D, Zank G, Zirnstein EJ.   +30 more
europepmc   +1 more source

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Solar magnetic fields

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.
exaly   +2 more sources

Magnetic fields in the solar photosphere

Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences, 2008
Recent high-resolution observations of the surface of the Sun have revealed the fine structure of a vast array of complex photospheric magnetic features. Observations of these magnetic field structures have already greatly enhanced our theoretical understanding of the interactions between magnetic fields and turbulent convection, and future ...
openaire   +3 more sources

Intermittency of the Solar Magnetic Field and Solar Magnetic Activity Cycle

Solar Physics, 2017
Small-scale solar magnetic fields demonstrate features of fractal intermittent behavior, which requires quantification. For this purpose we investigate how the observational estimate of the solar magnetic flux density \(B\) depends on resolution \(D\) in order to obtain the scaling \(\ln B_{D} = - k \ln D +a\) in a reasonably wide range. The quantity \(
A. S. Shibalova, V. N. Obridko, D. D. Sokoloff   +2 more
openaire   +1 more source

SOLAR MAGNETIC FIELDS

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.
openaire   +1 more source

Solar Magnetic Fields

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.
openaire   +1 more source

Magnetic fields and the solar corona

Solar Physics, 1970
Coronal magnetic fields calculated by the methods developed in Paper I (Altschuler and Newkirk, 1969) and the empirical description of the solar corona of November 1966 derived in Paper II (Newkirket al., 1970) are combined in order to investigate what connection exists between the magnetic fields and the density structure of the corona.
Gordon Newkirk, Martin D. Altschuler
openaire   +1 more source