Energy dissipation in substorms: plasmoids ejection

Silbergleit, V. M.; Artigas, Marta Maria Zossi; Manzano, J. R.

doi:10.1016/s1364-6826(96)00108-3

Cited by 2 publications

(4 citation statements)

References 11 publications

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“…There are different pathways for the dissipation of energy from geomagnetic storms (Weiss et al 1992;Slinker et al 1995;Silbergleit et al 1997;Lu et al 1998;Slavin et al 1998). The partitioning of the magnetic storm dissipation energy can be estimated using multiple techniques including ground and satellite-based observations of energy fluxes, empirical formulas (e.g., Pulkkinen et al 2002;Li et al 2012), model simulations (Palmroth et al 2004;Tanskanen et al 2005;Ngwira et al 2013), and assimilation techniques .…”

Section: Magnetic Storm Dissipationmentioning

confidence: 99%

“…The partitioning of the magnetic storm dissipation energy can be estimated using multiple techniques including ground and satellite-based observations of energy fluxes, empirical formulas (e.g., Pulkkinen et al 2002;Li et al 2012), model simulations (Palmroth et al 2004;Tanskanen et al 2005;Ngwira et al 2013), and assimilation techniques . In empirical methods, for example, estimates of the solar wind input energy, a function of solar wind speed and solar magnetic field orientation and strength (Silbergleit et al 1997) is used to determine the energy input into the magnetosphere (Gonzalez et al 1994;Pulkkinen et al 2002). In-situ measurements of the precipitation of auroral particles can be used in combination with auroral models to estimate magnetic storm energy.…”

Section: Magnetic Storm Dissipationmentioning

confidence: 99%

“…Numerous studies have estimated the power dissipation in magnetic storms (e.g., Akasofu 1978;Stern 1984;Akasofu & Kamide 1985;Weiss et al 1992;Lu et al 1995;Knipp et al 1998;Lu et al 1998;Baker et al 1997;Silbergleit et al 1997;Baker et al 2001;Pulkkinen et al 2002;Tanskanen et al 2002;Feldstein et al 2003;Palmroth et al 2004;Tanskanen et al 2005;Alex et al 2006;Guo et al 2011;Li et al 2012;Akasofu 2013). There is a wide range in dissipative energies due to the varying strength of the solar wind and geomagnetic indices, storm duration, as well as the technique used to derive the global power.…”

Section: Magnetic Storm Dissipationmentioning

confidence: 99%

See 2 more Smart Citations

Where does Earth’s atmosphere get its energy?

Kren

Pilewskie

Coddington

2017

J. Space Weather Space Clim.

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The Sun is Earth's primary source of energy. In this paper, we compare the magnitude of the Sun to all other external (to the atmosphere) energy sources. These external sources were previously identified in Sellers (1965); here, we quantify and update them. These external sources provide a total energy to the Earth that is more than 3700 times smaller than that provided by the Sun, a vast majority of which is provided by heat from the Earth's interior. After accounting for the fact that 71% of incident solar radiation is deposited into the earth system, the Sun provides a total energy to Earth that is still more than 2600 times larger than the sum of all other external sources.

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Section: Magnetic Storm Dissipationmentioning

confidence: 99%

Section: Magnetic Storm Dissipationmentioning

confidence: 99%

Section: Magnetic Storm Dissipationmentioning

confidence: 99%

See 1 more Smart Citation

Where does Earth’s atmosphere get its energy?

Kren

Pilewskie

Coddington

2017

J. Space Weather Space Clim.

View full text Add to dashboard Cite

show abstract

“…in the x-direction from 4...10 R E (Ieda et al, 1998) and 16.7 ± 13.0 R E (Moldwin and Hughes, 1992) up to 75...150 R E (Hones et al, 1984b), depending on their distance from the Earth. Estimations of the energy carried away by plasmoids have also varied by an order of magnitude, from about 0.2 × 10 15 J (Ieda et al, 1998) to 4 × 10 15 J (Silbergleit et al, 1997). In these studies plasmoids were detected mainly from the magnetic field and plasma data of ISEE-3 or Geotail spacecraft.…”

Section: Introductionmentioning

confidence: 99%

On large plasmoid formation in a global magnetohydrodynamic simulation

et al. 2011

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Abstract. We investigate plasmoid formation in the magnetotail using the global magnetohydrodynamic (MHD) simulation GUMICS-4. Here a plasmoid implies a major reconfiguration of the magnetotail where a part of the tail plasma sheet is ejected downstream, in contrast to small Earthwardpropagating plasmoids. We define a plasmoid based solely on the structure of the closed (connected to the Earth at both ends) magnetic field line region. In this definition a plasmoid is partly separated from the ordinary closed field line region by lobe field lines or interplanetary field lines resulting from lobe reconnection. We simulate an event that occurred on 18 February 2004 during which four intensifications of the auroral electroject (AE) index occurred in 8 h. Plasmoids form in the simulation for two of the four AE intensifications. Each plasmoid forms as a result of two consecutive large and fast rotations of the interplanetary magnetic field (IMF). In both cases the IMF rotates 180 degrees at 10 degrees per minute, first from southward to northward and some 15 min later from northward to southward. The other two AE intencifications however are not associated with a plasmoid formation. A plasmoid does not form if either the IMF rotation speed or the angular change of the rotation are small. We also present an operational definition for these fully connected plasmoids that enables their automatic detection in simulations. Finally, we show mappings of the plasmoid footpoints in the ionosphere, where they perturb the polar cap boundary in both hemispheres.

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Energy dissipation in substorms: plasmoids ejection

Cited by 2 publications

References 11 publications

Where does Earth’s atmosphere get its energy?

Where does Earth’s atmosphere get its energy?

On large plasmoid formation in a global magnetohydrodynamic simulation

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