Jove
Visualize
Contact Us
JoVE
x logofacebook logolinkedin logoyoutube logo
ABOUT JoVE
OverviewLeadershipBlogJoVE Help Center
AUTHORS
Publishing ProcessEditorial BoardScope & PoliciesPeer ReviewFAQSubmit
LIBRARIANS
TestimonialsSubscriptionsAccessResourcesLibrary Advisory BoardFAQ
RESEARCH
JoVE JournalMethods CollectionsJoVE Encyclopedia of ExperimentsArchive
EDUCATION
JoVE CoreJoVE BusinessJoVE Science EducationJoVE Lab ManualFaculty Resource CenterFaculty Site
Terms & Conditions of Use
Privacy Policy
Policies

Related Concept Videos

Magnetostatic Boundary Conditions01:28

Magnetostatic Boundary Conditions

1.1K
An electric field suffers a discontinuity at a surface charge. Similarly, a magnetic field is discontinuous at a surface current. The perpendicular component of a magnetic field is continuous across the interface of two magnetic mediums. In contrast, its parallel component, perpendicular to the current, is discontinuous by the amount equal to the product of the vacuum permeability and the surface current. Like the scalar potential in electrostatics, the vector potential is also continuous...
1.1K
Magnetic Field Lines01:19

Magnetic Field Lines

4.3K
The representation of magnetic fields by magnetic field lines is very useful in visualizing the strength and direction of the magnetic field. Each of the magnetic field lines forms a closed loop. The field lines emerge from the north pole (N), loop around to the south pole (S), and continue through the bar magnet back to the north pole.
Magnetic field lines follow several hard-and-fast rules:
4.3K
Torque Free Motion01:15

Torque Free Motion

561
The torque-free motion refers to the movement of a rigid body in space when no external torques are acting upon it. This type of motion can be observed in environments where there are no external forces or frictions, like in outer space. For example, a rotation of Mars in space is a torque-free motion. Mars is an axisymmetric object, meaning it has an axis of symmetry along which it rotates, designated as the z-axis. The rotating frame of reference is defined such that the center of mass of...
561
Kepler's First Law of Planetary Motion01:10

Kepler's First Law of Planetary Motion

4.2K
In the early 17th century, German astronomer and mathematician Johannes Kepler postulated three laws for the motion of planets in the solar system. He formulated his first two laws based on the observations of his forebears, Nikolaus Copernicus and Tycho Brahe.
Polish astronomer Nikolaus Copernicus put forth a theory that stated a heliocentric model for the solar system. According to this heliocentric theory, all the planets, including Earth, orbit the Sun in circular orbits.
On the other hand,...
4.2K
Magnetic Flux01:18

Magnetic Flux

3.7K
The magnetic flux measures the number of magnetic field lines passing through a given surface area. The SI unit for magnetic flux is the weber (Wb). Magnetic flux is a scalar quantity. It depends on three factors: the strength of the magnetic field B, the area through which the field lines pass, and the relative orientation of the field with the surface area.
Suppose a surface is divided into elements of area dA. For each element, the component of the magnetic field that is normal to the...
3.7K
Momentum And Radiation Pressure01:20

Momentum And Radiation Pressure

2.1K
An object absorbing an electromagnetic wave would experience a force in the direction of propagation of the wave. This force occurs because electromagnetic waves contain and transport momentum. The force accounts for the wave's radiation pressure exerted on the object. Maxwell's prediction was confirmed in 1903 by Nichols and Hull by precisely measuring radiation pressures with a torsion balance. The measuring instrument had mirrors suspended from a fiber kept inside a glass container.
2.1K

You might also read

Related Articles

Articles linked to this work by shared authors, journal, and citation graph.

Sort by
Same author

The Tandem Reconnection and Cusp Electrodynamics Reconnaissance Satellites (TRACERS) Mission.

Space science reviews·2025
Same author

Detection of visible-wavelength aurora on Mars.

Science advances·2025
Same author

Anomalous transient enhancement of planetary ion escape at Mars.

Nature communications·2025
Same author

The TRACERS Analyzer for Cusp Electrons.

Space science reviews·2025
Same author

Mass Supply from Io to Jupiter's Magnetosphere.

Space science reviews·2025
Same author

The Need for Near-Earth Multi-Spacecraft Heliospheric Measurements and an Explorer Mission to Investigate Interplanetary Structures and Transients in the Near-Earth Heliosphere.

Space science reviews·2024

Related Experiment Video

Updated: Sep 4, 2025

Scattering And Absorption of Light in Planetary Regoliths
11:34

Scattering And Absorption of Light in Planetary Regoliths

Published on: July 1, 2019

10.4K

Discrete Aurora at Mars: Dependence on Upstream Solar Wind Conditions.

Z Girazian1, N M Schneider2, Z Milby2

  • 1Department of Physics and Astronomy University of Iowa Iowa City IA USA.

Journal of Geophysical Research. Space Physics
|July 22, 2022
PubMed
Summary
This summary is machine-generated.

Mars

Keywords:
Marsauroradiscrete aurorasolar wind

More Related Videos

Experimental Methods of Dust Charging and Mobilization on Surfaces with Exposure to Ultraviolet Radiation or Plasmas
07:54

Experimental Methods of Dust Charging and Mobilization on Surfaces with Exposure to Ultraviolet Radiation or Plasmas

Published on: April 3, 2018

8.3K
Simulating Imaging of Large Scale Radio Arrays on the Lunar Surface
06:14

Simulating Imaging of Large Scale Radio Arrays on the Lunar Surface

Published on: July 30, 2020

5.0K

Related Experiment Videos

Last Updated: Sep 4, 2025

Scattering And Absorption of Light in Planetary Regoliths
11:34

Scattering And Absorption of Light in Planetary Regoliths

Published on: July 1, 2019

10.4K
Experimental Methods of Dust Charging and Mobilization on Surfaces with Exposure to Ultraviolet Radiation or Plasmas
07:54

Experimental Methods of Dust Charging and Mobilization on Surfaces with Exposure to Ultraviolet Radiation or Plasmas

Published on: April 3, 2018

8.3K
Simulating Imaging of Large Scale Radio Arrays on the Lunar Surface
06:14

Simulating Imaging of Large Scale Radio Arrays on the Lunar Surface

Published on: July 30, 2020

5.0K

Area of Science:

  • Planetary Science
  • Space Physics
  • Atmospheric Science

Background:

  • Discrete aurora on Mars are linked to particle precipitation in the upper atmosphere.
  • Observations by the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft since 2014 have provided extensive data on these auroras.
  • Previous studies indicated a sensitivity to the interplanetary magnetic field (IMF) clock angle near strong crustal magnetic fields.

Purpose of the Study:

  • To investigate the influence of various solar wind properties on the detection frequency of discrete Martian aurora.
  • To determine how solar wind dynamic pressure, IMF strength, and IMF cone angle affect aurora formation.
  • To differentiate the controlling factors of aurora occurrence inside and outside the strong crustal field region (SCFR).

Main Methods:

  • Utilizing ultraviolet discrete aurora observations from MAVEN's Imaging Ultraviolet Spectrograph (IUVS).
  • Correlating aurora data with upstream solar wind measurements from MAVEN.
  • Analyzing the relationship between aurora detection frequency and solar wind parameters (dynamic pressure, IMF strength, IMF clock and cone angles).

Main Results:

  • Outside the SCFR, aurora detection frequency increases with solar wind dynamic pressure and IMF strength, but is less sensitive to IMF orientation.
  • High dynamic pressure increases aurora occurrence but not brightness.
  • Inside the SCFR, aurora detection is moderately dependent on dynamic pressure and highly sensitive to IMF clock and cone angles, with specific orientations inhibiting aurora.

Conclusions:

  • Solar wind properties significantly influence discrete aurora formation at Mars.
  • The strong crustal field region exhibits distinct sensitivities to solar wind conditions compared to other areas.
  • This study provides the first comprehensive analysis of upstream solar wind impacts on Martian discrete aurora.