M. Stepanova(1), E. E. Antonova (2,3), C. Espinoza(1), A. Eyelade(1), N. Romanova (1), M. Martínez-Ledesma (1,4), J.A. Vadlivia(5), P. Moya (5), and V. Pinto (6)
(1) Universidad de Santiago de Chile, Chile (2) Lomonosov Moscow State University, Russian Federation (3) Space Research Institute RAS, Russian Federation (4) Universidad de Concepción, Chile (5) Universidad de Chile (6) University of New Hampshire, USA Wikipedia: Space physics is the study of plasmas as they occur naturally in the Earth's upper atmosphere (aeronomy) and within the Solar System. As such, it encompasses a far-ranging number of topics, such as heliophysics which includes the solar physics of the Sun: the solar wind, planetary magnetospheres and ionospheres, auroras, cosmic rays, and synchrotron radiation. Space physics is a fundamental part of the study of space weather and has important implications in not only to understanding the universe, but also for practical everyday life, including the operations of communications and weather satellites.
Some enigmas that propelled the birth of space physics
Why does the geomagnetic Why do comets have two tails? field have strong variations?
What causes the aurora? Geomagnetic Storm, Carrington Event, 1850.
The associated "white light flare" in the solar photosphere was observed and recorded by British astronomers Richard Carrington and Richard Hodgson. The storm caused strong auroral displays and wrought havoc with telegraph systems. March 1989 geomagnetic storm. 9 hour shut down for 6.000.000 people.
International Geophysical Year 1957-1958
First Russian Satellite, Sputnik 1, October 14 1957 Second Russian Satellite, Sputnik-2 November 3, 1957
S.N. Vernov (1910-1982) Explorer-3 launched March 26, 1958, weight 14.1 kg
J. Van Allen (1914-2006) The famous McIlwain’s group note
31 de enero 1958 3 de noviembre del 1957
Minitrack network to recieve the data from Explorer-1 Sputnik-3 launched May 15 1958, weight 1327 kg!
A.E. Chudakov (1921-2001) Discovery of the innet and outer radiation belts. The existence of the auroral oval, 1961, Olga Khorosheva
It should be a connection between the auroral oval and the outer radiation belt. Discovery of the Solar Wind
Vsekhsviatrsy, Nikolsky, Ponomarev, Cherednichenko (1955). С. К. Всехсвятский, Г. М. Никольский, Е. А. Пономарёв и В. И. Чередниченко, К вопросу о корпускулярном излучении Солнца (рус.) // Астрономический журнал. — 1955. — Т. 32. — С. 165.
Parker, Eugene N, (November 1958), "Dynamics of the Interplanetary Gas and Magnetic Fields". The Astrophysical Journal. 128: 664–676
Luna -1 (URSS). Launched January 1959 Group of Konstantin Gringauz from Space Research Institute (IKI) discovered the solar wind. Ulysses (NASA) 1990-2009. First measurements of the solar wind out of the ecliptic plane STEREO (NASA). Launched: 2006. For the first time we have a stereoscopic view of the solar wind.
Mission: Parker Solar Probe (NASA). Launched: August 2018 Goal: To discover the origins of the solar wind. Propiedades a 1 AU Ulysses Proton density 6.6 cm-3 Electron density 7.1 cm-3 He2+ density 0.25 cm-3 Bulk velocuty 450 km.s-1 Proton temperature 1.2x105 K Electron Temperature 1.4x105 K Magnetic field 7x10-9 T Travel time ~ 4 days Coronal mass ejections Geomagnetic field
Glatzmaier and Roberts, (UCLA, 2006) Intrinsic magnetosphere Induced magnetosphere Planeta Campo Misiones magn. Mercury yes Mariner 10 (NASA,1974), BepiColombo (ESA, JAXA, 2018) Venus no Venera 3-16 (URSS, años 60-80), Pioneer Venus (NASA, 1972), VEGA (URSS, 1985), Venus Express (ESA, 2008), Planet C (JAXA, 2010) Earth si Ahora: Cluster, Themis, MMS, Van Allen Probes, DMSP, etc SUCHAI Mars no Mars Odyssey (NASA), Mars Express (ESA), Mars Reconnaisance Orbiter (NASA) Jupiter si Juno (NASA, 2016) Uranus si flyby only: Voyager 2 Neptune si flyby only: Voyager 2 Importance of the intrinsic magnetosphere for the origins of life
Jim Green (NASA) proposed to create an artificial magnetosphere on Mars. Mars 3.800.000.000 years ago? Heliosphere
L.L. Orionis stellar wind Exoplanetary magnetospheres
LOFAR telescopes should be able to detect the auroral kilometric radiation generated by exoplanetary aurora.
Hale telescope: HR 8799 star Measurements in space (example of the THEMIS mission): Dungey, 1961. Importance of reconnection.
Dynamics Explorer, Frank et al. 1974 Hannes Alfvén (1908-1995) Nobel Price 1970
The balance of the total plasma pressure in the magnesphere should be fulfilled at least at the large and medium scales even in the presence of turbulence.
Pressure balance at the magnetopause McFadden et al Space Sci. Rew. (2008)
Pressure should be important for the space weather forecast Evidences of the turbulence in the magnetosphere Velocity and magnetic field fluctuations are studied by Angelopoulos et al. (1992, 1993, 1996, 1999); Borovsky et al. (1997, 1998), Antonova et al. (2000, 2002); Ovchinnikov et al. (2002), Neagu et al. (2001, 2002); Troshichev et al. (2001, 2002); Petrukovich and Yermolaev (2002); Borovsky and Funsten (2003a,b); Voros et al. (2003); Volwerk et al. (2004); Goldstein (2005); Weygand et al. (2005); Stepanova et al. (2005, 2009,2011, 2012) etc.
ISEE-2 results Interball/Tail probe results (Angelopoulos et al., 1993) (Antonova et al., 2000, 2002) Antonova and Ovchinnikov, JGR (1999)
How to stabilize the turbulent plasma sheet?
A balance between the regular and turbulent transports (Antonova and Ovchinnikov, 1996, 1997, 1999)
A total pressure balance across the geomagnetic tail (Michalov et al. [1968], Stiles [1978], Spence et al. [1989], Tsyganenko [1990], Baumjohann et al. [1990], Kistler et al. [1993], Petrukovich [1999], Tsyganenko and Mukai [2003]) Stepanova and Antonova, JASTP (2011) Superdarn Cluster vertical crossing
September 12, 2004
Stepanova, Espinoza work in progress Themis mission. February 22, 2008
Turbulence in the plasma sheet in MHD simulations [El-Alaoui et al., 2010, 2012].
-3 IMF Bz=-5 nT, nsw=20 cm , Vx=500 km/s. Particle distribution functions in space plasmas are not Maxwellian Eyelade, Espinoza, Stepanova, Moya et al., 2021 submitted to Frontiers in Astronomy and Space Science The relation between the turbulence and kappa index is not the same for high and low beta plasma and along and across the magnetic field Quite auroral arcs and constantly observed in the auroral oval. If the plasma sheet is turbulent, why the auroral arcs are so quiet?
Bright auroral arcs are Physics of Auroral Arc Formation, ed. S.-I. observed for hours without Akasofu, J.R. Kan, Geophysical monograph 25, 1981 The polar aurora; woodcut by changing their forms. Fridtjof Nansen. The lines defining the “curtains” of the auroral arcs follow Are they mapped into the magnetic field lines. plasma sheet? Rough classification of previous studies: Low-orbting satellites High-orbiting satellites
Statistical studies
Event oriented studies D e M i c h e l i s e t a l . Do the quiet time pressure [ 1 9 9 9 ] profiles match? Stepanova et al, ASR, 2008
There are evidences that the solar wind dynamic pressure can directly drive the pressure inside the magnetosphere June 1-5, 2013 geomagnetic storm (DOY 152-156) 2d tracking of the inner magnetosphere plasma pressure during 1 June 2013 storm
NOAA 15-19, METOP 1-2, POES/TED instrument. Dipole mapping
6 hours averaging DMSP POES 1-5 June storm
Time interval used for averaging Plasma pressure increases just before and during the main phase of the storm. Plasma pressure inside the magnetosphere follows the solar wind dynamic pressure Stepanova et al., JASTP, 2020, the same June 1-5 geomagnetic storm.
The use of high-orbiting satellites allowed us to see how the position and the value of maximim pressure changes during the storm.
The pressure reaches the maximum value at the end of the main phase. At the same time the maximum has the closest to the Earth position. Prediction of the closest to the Earth location of the maximum of electron fluxes in a new outer radiation belt (Tverskaya relation) for the minimal
Dst=-105 nT ⟹ Lmin=4.02.
Intensity of the westward auroral electrojet, obtained using the IMAGE magnetometer network near the Dst minimum. The 1D equivalent current system obtained using the data of the IMAGE magnetometer network on 8–9 October 2012 Stepanova et al., JASTP, 2020, the same June 1-5 geomagnetic storm.
Tverskaya relation:
Lpred = 3.89
Analysis of energetic electron spectra showed that the power law index changes during the storm reaching the maximum absolute value at the end of the main phase. An increase of the power law index after the main phase of the storm can be related to an increase of the losses as the electron energy increases, and/or to the processes of relaxation of the electron distribution functions due to increase of the turbulent fluctuations in a wide range of scales and frequenies. Variation of plasma pressure Wing at al., JGR, 2013 during substorms
Statistical studies showed that the plasma pressure increases before an onset and during the expansion phase of isolated substorms. Plasma pressure profiles from a single satellite
S t e p a n o v a e t a l , J G R , 2 0 0 2
Advantage: - The possibility to obtain a full radial profile during a few minutes
Disadvantage: - We measure only a portion of pressure -Correct consideration of the field-aligned potential drop - Mapping involves a geomagnetic field model
Possibility to use the plasma pressure as a natural tracer. But a substorms develops too fast. How the plasma pressure behaves during isolated substorms. DMSP mission: Typically four satellites at time. Good time and some MLT coverage. I s o l a t e d s u b s t o r m 2 0 0 8 / 1 2 / 2 2
Positions of the plasma pressure maximums Plasma pressure follows the solar wind dynamic pressure up to the end of the expansion phase Conclusions: The discovery of the exoplanetary magnetospheres is a matter of years. The knoweledge of the history of the discovery of our own magnetosphere would be helpful to get an idea what to expect. In our opinion the key processes to consider would be the total pressure balance inside the turbulent wake.