Zobrazeno 1 - 10
of 101 191
pro vyhledávání: '"A, Strahl"'
Autor:
Owen, Christopher J.1 (AUTHOR) c.owen@ucl.ac.uk, Abraham, Joel Baby1 (AUTHOR), Nicolaou, Georgios1 (AUTHOR), Verscharen, Daniel1 (AUTHOR), Louarn, Philippe2 (AUTHOR), Horbury, Timothy S.3 (AUTHOR)
Publikováno v:
Universe (2218-1997). Oct2022, Vol. 8 Issue 10, pN.PAG-N.PAG. 15p.
Autor:
Jeong, Seong-Yeop, Abraham, Joel B., Verscharen, Daniel, Berčič, Laura, Stansby, David, Nicolaou, Georgios, Owen, Christopher J., Wicks, Robert T., Fazakerley, Andrew N., Rueda, Jeffersson A. Agudelo, Bakrania, Mayur
We analyze the micro-kinetic stability of the electron strahl in the solar wind depending on heliocentric distance. The oblique fast-magnetosonic/whistler (FM/W) instability has emerged in the literature as a key candidate mechanism for the effective
Externí odkaz:
http://arxiv.org/abs/2201.09610
We present a kinetic stability analysis of the solar wind electron distribution function consisting of the Maxwellian core and the magnetic-field aligned strahl, a superthermal electron beam propagating away from the sun. We use an electron strahl di
Externí odkaz:
http://arxiv.org/abs/2107.08127
Autor:
Cattell, C., Breneman, A., Dombeck, J., Hanson, E., Johnson, M., Halekas, J., Bale, S. D., de Wit, T. Dudok, Goetz, K., Goodrich, K., Malaspina, D., Pulupa, M., Case, T., Kasper, J. C., Larson, D., Stevens, M., Whittlesey, P.
Using the Parker Solar Probe FIELDS bandpass filter data and SWEAP electron data from Encounters 1 through 9, we show statistical properties of narrowband whistlers from ~16 Rs to ~130 Rs, and compare wave occurrence to electron properties including
Externí odkaz:
http://arxiv.org/abs/2111.03619
Autor:
Macneil, Allan R.1 (AUTHOR) a.r.macneil@reading.ac.uk, Owens, Mathew J.1 (AUTHOR), Lockwood, Mike1 (AUTHOR), Štverák, Štěpán2,3 (AUTHOR), Owen, Christopher J.4 (AUTHOR)
Publikováno v:
Solar Physics. Feb2020, Vol. 295 Issue 2, p1-26. 26p.
Autor:
Jagarlamudi, V. K., de Wit, T. Dudok, Froment, C., Krasnoselskikh, V., Larosa, A., Bercic, L., Agapitov, O., Halekas, J. S., Kretzschmar, M., Malaspina, D., Moncuquet, M., Bale, S. D., Case, A. W., Kasper, J. C., Korreck, K. E., Larson, D. E., Pulupa, M., Stevens, M. L., Whittlesey, P.
Publikováno v:
A&A 650, A9 (2021)
We studied the properties and occurrence of narrow band whistler waves and their interaction with strahl electrons observed between 0.17 and 0.26 au during the first encounter of Parker Solar Probe. We observe that occurrence of whistler waves is low
Externí odkaz:
http://arxiv.org/abs/2101.06723
Autor:
Bercic, Laura, Larson, Davin, Whittlesey, Phyllis, Maksimovic, Milan, Badman, Samuel T., Landi, Simone, Matteini, Lorenzo, Bale, Stuart. D., Bonnell, John W., Case, Anthony W., de Wit, Thierry Dudok, Goetz, Keith, Harvey, Peter R., Kasper, Justin C., Korreck, Kelly E., Livi, Roberto, MacDowall, Robert J., Malaspina, David M., Pulupa, Marc, Stevens, Michael L.
The shape of the electron velocity distribution function plays an important role in the dynamics of the solar wind acceleration. Electrons are normally modelled with three components, the core, the halo, and the strahl. We investigate how well the fa
Externí odkaz:
http://arxiv.org/abs/2003.04016
We develop a kinetic theory for {the electron strahl, a beam of energetic electrons which propagate} from the sun along the Parker-spiral-shaped magnetic field lines. By assuming a Maxwellian electron distribution function in the near-sun region wher
Externí odkaz:
http://arxiv.org/abs/1908.01902
Autor:
Verscharen, Daniel, Chandran, Benjamin D. G., Jeong, Seong-Yeop, Salem, Chadi S., Pulupa, Marc P., Bale, Stuart D.
Publikováno v:
Astrophys. J. 886, 2, 2019
We investigate the scattering of strahl electrons by microinstabilities as a mechanism for creating the electron halo in the solar wind. We develop a mathematical framework for the description of electron-driven microinstabilities and discuss the ass
Externí odkaz:
http://arxiv.org/abs/1906.02832
Electron velocity distribution functions in the solar wind according to standard models consist of 4 components, of which 3 are symmetric - the core, the halo, and the superhalo, and one is magnetic field-aligned, beam-like population, referred to as
Externí odkaz:
http://arxiv.org/abs/1904.08272