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3 edition of Determination of coronal magnetic fields from vector magnetograms found in the catalog.

Determination of coronal magnetic fields from vector magnetograms

Determination of coronal magnetic fields from vector magnetograms

second year progress report

  • 178 Want to read
  • 12 Currently reading

Published by Science Applications International Corp., National Aeronautics and Space Administration, National Technical Information Service, distributor in San Diego, Calif, [Washington, DC, Springfield, Va .
Written in English

    Subjects:
  • Cosmic magnetic fields.,
  • Sun -- Corona -- Magnetic fields.

  • Edition Notes

    StatementZoran Mikic ; principal investigator.
    SeriesNASA contractor report] -- NASA CR-194744., NASA contractor report -- NASA CR-194744.
    ContributionsUnited States. National Aeronautics and Space Administration.
    The Physical Object
    FormatMicroform
    Pagination1 v.
    ID Numbers
    Open LibraryOL14702502M

    The million-degree solar corona is the basis for the solar wind and the Sun's X-ray emission. Two decades ago space observations ruled out what was then the established explanation for coronal heating: that it was a consequence of acoustic waves generated in the photospheric convection and propagating up into the corona where they were damped by viscosity, thermal conductivity, and shock. Title: The vector magnetic and Doppler velocity fields at the cancellation sites Abstract: Spatial structures and time evolutions of the vector magnetic and Doppler velocity fields around the magnetic cancellatoin sites are studied by using the Hinode SOT Spectropolarimeter (SP) and Filtergrams (FG). Two senarios, i.e. the "U-loop emergence.

    A Doppler width delta lambda (D) - 25mA is bound to be consistent with a low spot temperature and microturbulence, and a damping constant of a = Title: The inference of vector magnetic fields from polarization measurements with limited spectral resolution Authors: Lites, B. W.; Skumanich, A. Altcode: A. The magnetic field vector of the Sun-as-a-star - II. Evolution of the large-scale vector field through activity cy Monthly Notices of the Royal Astronomical Society .

    A01 – Planetary Magnetic Fields and Secular Variations. Convener: Ingo Wardinski (France) Co-Conveners: Phil Livermore (UK), Nicolas Gillet (France), Daniel Lathrop (USA), Sanja Panovska (Germany), Rachel Bailey (Austria), Ciaran Beggan (UK) Description. Magnetic fields are a fundamental characteristic of the Earth and other planetary bodies, whose diverse structures are the manifestation. Model for the Coupled Evolution of Subsurface and Coronal Magnetic Fields in Solar Active Regions 33 A&A A Archontis, V.; Hood, A. W.; Brady, C.


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Determination of coronal magnetic fields from vector magnetograms Download PDF EPUB FB2

Get this from a library. Determination of coronal magnetic fields from vector magnetograms: progress report. [Zoran Mikic; United States.

National Aeronautics and Space Administration.]. Get this from a library. Determination of coronal magnetic fields from vector magnetograms: final progress report. [Zoran Mikic; United States.

National Aeronautics and Space Administration.]. 3D Coronal magnetic field from vector magnetograms: non-constant. force-free configuration of the active region NOAA Article (PDF Available) in Astronomy and Astrophysics (3) September.

@article{osti_, title = {Image-optimized Coronal Magnetic Field Models}, author = {Jones, Shaela I. and Uritsky, Vadim and Davila, Joseph M., E-mail: [email protected], E-mail: [email protected]}, abstractNote = {We have reported previously on a new method we are developing for using image-based information to improve global coronal magnetic field models.

The structure and dynamics of the solar corona is dominated by the magnetic field. In most areas in the corona magnetic forces are so dominant that all non-magnetic forces like plasma pressure gradient and gravity can be neglected in the lowest order. This model assumption is called the force-free field assumption, as the Lorentz force vanishes.

This can be obtained by either vanishing Cited by: Non-force-free extrapolation of solar coronal magnetic field using vector magnetograms Article in Journal of Atmospheric and Solar-Terrestrial Physics 72(2) February with 37 Reads.

Miki´c, Z. and McClymont, A.N.,“Deducing coronal magnetic fields from vector magnetograms”, in Solar Active Region Evolution: Comparing Models with Observations, Proceedings of the 14th In-ternational Summer Workshop, NSO / Sacramento Peak, Sunspot, New Mexico, USA, 30 August–3Cited by: Measurements of magnetic fields and electric currents in the pre-eruptive corona are crucial to study solar eruptive phenomena, like flare and coronal mass.

Read While You Wait - Get immediate ebook access* when you order a print book Earth Large Scale Solar Magnetic Fields and Their Consequences. Pages Preliminary Results of Spectroscopic Determination of the Coronal Rotation. Pages Brand: Springer Netherlands. Dynamic Evolution of Emerging Magnetic Flux Tubes in the Solar Convective Envelope Y.

Fan 30 Coupling of Convective Flows and Emerging Magnetic Fields Fang, Fang, Manchester IV, Ward, Abbett, William P., van der Holst, Bart 31 Statistical Analysis of Brightenings near Coronal Hole Boundaries Farid, S., Winebarger, A., Lionello, R., Titov, R.

32 iii. @article{osti_, title = {Statistical study of free magnetic energy and flare productivity of solar active regions}, author = {Su, J. and Jing, J. and Wang, S. and Wang, H.

and Wiegelmann, T., E-mail: [email protected]}, abstractNote = {Photospheric vector magnetograms from the Helioseismic and Magnetic Imager on board the Solar Dynamic Observatory are utilized as the boundary. Our NLFF codes are installed to NASA-Space Weather Lab., Community Coordinated Modelling Center (CCMC).

NLFF is a Non-Linear Force Free coronal magnetic field model. Mikic (I, 25m): Deducing Coronal Magnetic Fields from Vector Magnetograms Altrock: Solar Coronal Structure: A Comparison of NSO/SP Ground- Based Coronal Emission Line Intensities and Temperatures with Yohkoh SXT and WCO Magnetic Field Data Kocharov: Temporal and Spatial Evolution of the Solar Magnetic Field: A View from the Sidelines.

1 Introduction. Coronal mass ejections (CMEs) are large clouds of plasma and magnetic flux expelled from the Sun into the heliosphere. If directed toward Earth, they can cause significant space weather effects upon impact with the near‐Earth by: The FIELDS instrument (Bale et al.

) measures DC-coupled magnetic and electric fields, plasma wave magnetic and electric fields, and solar radio emissions. From the measured local electric and magnetic fields, it produces an estimate of the Poynting flux, i.e., the electromagnetic energy flux crossing that region of space.

The topology and dynamics of the three-dimensional magnetic field in the solar atmosphere govern various solar eruptive phenomena and activities, such as flares, coronal mass ejections, and filaments/prominences. We have to observe and model the vector magnetic field to understand the structures and physical mechanisms of these solar by: In this sense, changes in AR magnetic field can be used to unveil other relevant features like plasma flows in the region.

Here, observations of surface 3D vector magnetic field from SDO/HMI are studied with the differential affine velocity estimator for vector magnetograms (DAVE4VM) to recover 3D plasma flows in the photosphere.

Photospheric magnetograms show that coronal holes are more unipolar than other regions; i.e., they have a larger degree of magnetic flux imbalance between the two polarities (Levine, ; Wang, ).

For the large polar coronal holes, this appears to be the long-term outcome of the decay of active-region magnetic fields and their eventual. The only information about the magnetic helicity of the sun available to date is from surface magnetic fields, and these data are necessarily incomplete.

Nevertheless, some systematic trends can be identified. Vector magnetograms of active regions show negative (positive) current helicity in the northern (southern) hemisphere. From local Cited by: explosions of the solar magnetic field and matter known as coronal mass ejections/eruptive flares.

Those events also produce the most destructive space weather at Earth, with damaging consequences ranging from communication and GPS blackouts to the loss of high-orbiting satellites and. Determination of Coronal Rotation from XBPs Observed with Hinode/XRT: (vector) magnetograms. As the magnetic fields in the solar surface provides the information on the formation of magnetic field in the subatmosphere, the statistical analysis of the observational magnetic helicity is also important for the confirmation of the solar dynamo.

Magnetic Reconnection and Hard X-ray Energetics in dozens of Two-ribbon Flares: Ewan Dickson: Poster: Simulations and Testing of STIX Software: Santiago Vargas Dominguez: Poster: Study of magnetic field variations in high-cadence vector magnetograms during solar flares: Li Feng: Poster: A new tool for automated CME detection and tracking using.It is shown that the fast magnetic reconnection in the current sheet below the flux rope in combination with outward curvature forces results in a fast ejection of the flux rope as observed for solar CMEs.

The results are compared for both background magnetic fields, i.e. the dipole field and the solar wind model.