с 01.01.2013 по настоящее время
Иркутск, Россия
с 01.01.2010 по настоящее время
Иркутск, Иркутская область, Россия
In recent years, information about the distance between the body of rapid coronal mass ejection (CME) and the associated shock wave has been used to measure the magnetic field in the solar corona. In all cases, this tech-nique allows us to find coronal magnetic field radial profiles B(R) applied to the directions almost perpendicular to the line of sight. We have determined radial distributions of magnetic field strength along the directions close to the Sun–Earth axis. For this purpose, using the “ice-cream cone” model and SOHO/LASCO data, we found 3D characteristics for fast halo coronal mass ejections (HCMEs) and for HCME-related shocks. With these data we managed to obtain the B(R) distributions as far as ≈43 solar radii from the Sun’s center, which is approximately twice as far as those in other studies based on LASCO data. We have concluded that to improve the accuracy of this method for finding the coronal magnetic field we should develop a technique for detecting CME sites moving in the slow and fast solar wind. We propose a technique for selecting CMEs whose central (paraxial) part actually moves in the slow wind.
CME, shock, solar wind, magnetic field
1. Artsimovich L.A., Sagdeev R.Z. Fizika plazmy dlya fizikov [Plasma physics for physicists]. Moscow, Atomizdat. 1979, 320 p. (In Russian).
2. Bemporad A., Mancuso S. First complete determination of plasma physical parameters across a coronal mass ejection-driven shock. Astrophys. J. 2010, vol. 720, pp. 130-143. DOI:https://doi.org/10.1088/0004-637X/720/1/130.
3. Brueckner G.E., Howard R.A., Koomen M.J., Korendyke C.M., Michels D.J., Moses J.D. The Large Angle Spectroscopic Coronagraph (LASCO). Solar Phys. 1995, vol. 162, pp. 357-402. DOI:https://doi.org/10.1007/BF00733434.
4. Bogod V.M., Yasnov L.V. Determination of the structure of the coronal magnetic field using microwave polarization measurements. Solar Phys. 2016, vol. 291, pp. 3317-3328.
5. Cho K.-S., Lee J., Gary D.E., Moon Y.-J., Park Y.D. Magnetic field strength in the solar corona from type II band splitting. Astrophys. J. 2007, vol. 665, p. 799.
6. Fainshtein V.G. The interaction effect of fast and slow solar wind streams in interplanetary space on wind characteristics at the Earth’s orbit. Solar Phys. 1991, vol. 136, pp. 169-189. DOI:https://doi.org/10.1007/BF00151702.
7. Fainshtein V.G. Method for determining the parameters of full halo coronal mass ejections. Geomagnetism and Aeronomy. 2006, vol. 46, iss. 3, pp. 339-349. DOI:https://doi.org/10.1134/S00167932 0603008X.
8. Fainshtein V.G., Egorov Ya.I. Origin of a CME-related shock within the LASCO C3 field-of-view. Eprint arXiv.2017. arXiv:1712.09051.
9. Gopalswamy N., Yashiro S. The strength and radial profile of the coronal magnetic field from the standoff distance of a coronal mass ejection-driven shock. Astrophys. J. Lett. 2011, vol. 736, article id. L17, 5 p. DOI:https://doi.org/10.1088/2041-8205/736/ 1/L17.
10. Gopalswamy N., Akiyama S., Yashiro S., Michalek G., Lepping R.P. Solar sources and geospace consequences of interplanetary magnetic clouds observed during solar cycle 23. J. Atmos. Solar-Terr. Phys. 2008, vol. 70, p. 245.
11. Howard R.A., Moses J.D., Vourlidas A., et al. Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI). Space Sci. Rev. 2008, vol. 136, iss. 1-4. pp. 67-115. DOI: 10.1007/ s11214-008-9341-4.
12. Ingleby L.D., Spangler S.R., Whiting C.A. Probing the large-scale plasma structure of the solar corona with Faraday rotation measurements. Astrophys. J. 2007, vol. 668, p. 520.
13. Kaiser M.L., Kucera T.A., Davila J.M., St. Cyr O.C., Guhathakurta M., Christian E. The STEREO mission: an introduction. Space Sci. Rev. 2008, vol. 136, pp. 5-16. DOI: 10.1007/ s11214-007-9277-0.
14. Kim T., Moon Y., Na H. Comparison of CME radial velocities from a flux rope model and an ice cream cone model. American Geophysical Union, Fall Meeting 2011, abstract #SH51A-1992.
15. Kim R.-S., Gopalswamy N., Moon Y.-J., Cho K.-S., Yashiro S. Magnetic field strength in the upper solar corona using white-light shock structures surrounding coronal mass ejections. Astrophys. J. 2012, vol. 746, article id. 118, 8 p. DOI: DOI:https://doi.org/10.1088/0004-637X/746/2/118.
16. Landau L.D., Lifshitz E.M. Gidrodinamika [Fluid mechanics]. 1988, 733 p. (In Russian).
17. Leblanc Y., Dulk G.A., Bougeret J.-L. Tracing the electron density from the corona to 1 au. Solar Phys. 1998, vol. 183, pp. 165-180. DOI:https://doi.org/10.1023/A:1005049730506.
18. Lee J. Radio emissions from solar active regions. Space Sci. Rev. 2007, vol. 133, pp. 73-102. DOI:https://doi.org/10.1007/s11214-007-9206-2.
19. Lin H., Penn M.J., Tomczyk S. A new precise measurement of the coronal magnetic field strength. Astrophys. J. 2000, vol. 541, pp. L83-L86. DOI:https://doi.org/10.1086/312900.
20. Manchester W.B., Gombosi T.I., Roussev I., Ridley A., de Zeeuw D.L., Sokolov I.V., Powell K.G., Tóth G. Modeling a space weather event from the Sun to the Earth: CME generation and interplanetary propagation. J. Geophys. Res.: Space Phys. 2004, vol. 109, A02107.
21. Mann G., Klassen A., Estel C., Thompson B.J. Coronal transient waves and coronal shock waves. 8th SOHO Workshop “Plasma Dynamics and Diagnostics in the Solar Transition Region and Corona”: Proc. Paris, 1999, pp. 477-481.
22. Michalek G. An asymmetric cone model for halo coronal mass ejections. Solar Phys. 2006, vol 237, iss. 1, pp. 101-118. DOI:https://doi.org/10.1007/s11207-006-0075-8.
23. Pӓtzold M., Bird M.K., Volland H., Levy G.S., Seidel B.L., Stelzried C.T. The mean coronal magnetic field determined from HELIOS Faraday rotation measurements. Solar Phys. 1987, vol. 109, pp. 9-105. DOI: 10.1007/ BF00167401.
24. Poomvises W., Gopalswamy N., Yashiro S., Kwon R.-Y., Olmedo O. Determination of the heliospheric radial magnetic field from the standoff distance of a CME-driven shock observed by the STEREO spacecraft. Astrophys. J. 2012, vol. 758, article id. 118, 6 p. DOI:https://doi.org/10.1088/0004-637X/758/2/118.
25. Rudenko G.V. Extrapolation of the solar magnetic field within the potential-field approximation from full-disk magnetograms. Solar Phys. 2001, vol. 198, pp. 5-30. DOI: 10.1023/ A:1005270431628.
26. Rudenko G.V., Myshyakov I.I. Analysis of reconstruction methods for nonlinear force-free fields. Solar Phys. 2009, vol. 257, pp. 287-304. DOI:https://doi.org/10.1007/s11207-009-9389-7.
27. Russell C.T., Mulligan T. On the magnetosheath thicknesses of interplanetary coronal mass ejections. Planet. Space Sci. 2002, vol. 50, pp. 527-534. DOI:https://doi.org/10.1016/S0032-0633(02) 00031-4.
28. Sahal-Bréchot S., Malinovsky M., Bommier V. The polarization of the O VI 1032 Å. Astron. Astrophys. 1986, vol. 168, pp. 284-300.
29. Sheeley N.R., Jr., Wang Y.-M., Hawley S.H., et al. Measurements of flow speeds in the corona between 2 and 30 R. Astrophys. J. 1997, vol. 484, pp. 472-478. DOI:https://doi.org/10.1086/304338.
30. Sheeley N.R., Hakala W.N., Wang Y.-M. Detection of coronal mass ejection associated shock waves in the outer corona. J. Geophys. Res. 2000, vol. 105, pp. 5081-5092. DOI:https://doi.org/10.1029/1999JA000338.
31. Schmidt J.M., Cairns I.H., Gopalswamy N., Yashiro S. Coronal magnetic field profiles from shock-CME standoff distances. J. Geophys. Res.: Space Phys. 2016, vol. 121, pp. 9299-9315. DOI:https://doi.org/10.1002/2016JA022956.
32. Schwenn R., Marsch E. (Eds.) Physics of the Inner Heliosphere I. Large-Scale Phenomena. Springer-Verlag, 1990, 293 p. DOI:https://doi.org/10.1007/978-3-642-75361-9.
33. Spangler S.R. The strength and structure of the coronal magnetic field. Space Sci. Rev. 2005, vol. 121, pp. 189-200. DOI:https://doi.org/10.1007/s11214-006-4719-7.
34. Thernisien A.F.R., Howard R.A., Vourlidas A. Modeling of flux rope coronal mass ejections. Astrophys. J. 2006, vol. 652, pp. 763-773. DOI:https://doi.org/10.1086/508254.
35. Wiegelmann T. Nonlinear force-free modeling of the solar coronal magnetic field. J. Geophys. Res. 2008, vol. 113, A03S02. DOI:https://doi.org/10.1029/2007JA012432.
36. Xue X.H., Wang C.B., Dou X.K. An ice-cream cone model for coronal mass ejections. J. Geophys. Res.: Space Phys. 2005, vol. 110, iss. A8, CiteID A08103. DOI:https://doi.org/10.1029/2004JA010698.
37. URL: https://cdaw.gsfc.nasa.gov/CME_list/HALO/halo.html (accessed September 16, 2017).
38. URL: http://wso.stanford.edu/synsourcel.html (accessed September 16, 2017).
39. URL: http://wso.stanford.edu/synoptic/WSO-S.2107.gif (accessed September 16, 2017).
