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

Magnetic Fields01:27

Magnetic Fields

7.1K
A moving charge or a current creates a magnetic field in the surrounding space, in addition to its electric field. The magnetic field exerts a force on any other moving charge or current that is present in the field. Like an electric field, the magnetic field is also a vector field. At any position, the direction of the magnetic field is defined as the direction in which the north pole of a compass needle points.
A magnetic field is defined by the force that a charged particle experiences...
7.1K
Magnetic Field Lines01:19

Magnetic Field Lines

5.4K
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:
5.4K
Magnetostatic Boundary Conditions01:28

Magnetostatic Boundary Conditions

1.6K
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...
1.6K
Magnetic Field of a Solenoid01:18

Magnetic Field of a Solenoid

5.6K
A solenoid is a conducting wire coated with an insulating material, wound tightly in the form of a helical coil. The magnetic field due to a solenoid is the vector sum of the magnetic fields due to its individual turns. Therefore, for an ideal solenoid, the magnetic field within the solenoid is directly proportional to the number of turns per unit length and the current. Conversely, the magnetic field outside the solenoid is zero.
Consider a solenoid with 100 turns wrapped around a cylinder of...
5.6K
Magnetic Declination01:19

Magnetic Declination

369
Magnetic declination is the angle between true north, which aligns with the Earth's rotational axis, and magnetic north, which follows the direction of the Earth's magnetic field. This discrepancy exists because the magnetic poles do not coincide with the geographic poles. The value of magnetic declination depends on the observer's location on Earth and is subject to changes over time due to the dynamic nature of the Earth's magnetic field.The declination is called eastern when magnetic north...
369
Divergence and Curl of Magnetic Field01:26

Divergence and Curl of Magnetic Field

3.9K
The magnetic field due to a volume current distribution given by the Biot–Savart Law can be expressed as follows:
3.9K

You might also read

Related Articles

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

Sort by
Same authorSame journal

Investigating the Relationship Between Physical Properties and Spatial Irregularities at Coronal Hole Boundaries.

Solar physics·2026
Same authorSame journal

A Geomagnetic Estimate of Heliospheric Modulation Potential over the Last 175 Years.

Solar physics·2026
Same author

A near-real-time data-assimilative model of the solar corona.

Science (New York, N.Y.)·2025
Same author

Sun-like stars produce superflares roughly once per century.

Science (New York, N.Y.)·2024
Same author

Combined Surface Flux Transport and Helioseismic Far-Side Active Region Model (FARM).

Solar physics·2024
Same author

The Sun's differential rotation is controlled by high-latitude baroclinically unstable inertial modes.

Science advances·2024
Same journal

The Behaviour of the EUV Corona Before Flares in Regions with High Free Magnetic Energy.

Solar physics·2026
Same journal

SSTrack: An Automatic Sunspot Identification and Tracking Algorithm to Support the Measurement of Sunspot Rotation.

Solar physics·2026
Same journal

Solar Cycle Variation of Sustained Gamma Ray Emission from the Sun.

Solar physics·2026
Same journal

The EUV Late-Phase: Statistical Results from 15 Years of Solar Dynamics Observatory Observations.

Solar physics·2026
See all related articles

Related Experiment Video

Updated: Jan 11, 2026

Surface Mapping of Earth-like Exoplanets using Single Point Light Curves
06:48

Surface Mapping of Earth-like Exoplanets using Single Point Light Curves

Published on: May 10, 2020

3.9K

Evaluating Solar Wind Forecast Using Magnetic Maps That Include Helioseismic Far-Side Information.

Stephan G Heinemann1,2, Dan Yang3, Shaela I Jones4

  • 1Institute of Physics, University of Graz, Universitätsplatz 5, 8010 Graz, Austria.

Solar Physics
|November 13, 2025
PubMed
Summary
This summary is machine-generated.

Accurately forecasting space weather requires understanding the Sun's magnetic field. Incorporating far-side solar data from helioseismology significantly improves solar wind predictions and heliospheric models.

Keywords:
Active regionsMagnetic fieldsSolar wind

More Related Videos

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

5.3K
Surface Renewal: An Advanced Micrometeorological Method for Measuring and Processing Field-Scale Energy Flux Density Data
09:55

Surface Renewal: An Advanced Micrometeorological Method for Measuring and Processing Field-Scale Energy Flux Density Data

Published on: December 12, 2013

9.1K

Related Experiment Videos

Last Updated: Jan 11, 2026

Surface Mapping of Earth-like Exoplanets using Single Point Light Curves
06:48

Surface Mapping of Earth-like Exoplanets using Single Point Light Curves

Published on: May 10, 2020

3.9K
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

5.3K
Surface Renewal: An Advanced Micrometeorological Method for Measuring and Processing Field-Scale Energy Flux Density Data
09:55

Surface Renewal: An Advanced Micrometeorological Method for Measuring and Processing Field-Scale Energy Flux Density Data

Published on: December 12, 2013

9.1K

Area of Science:

  • * Heliophysics and space weather research.
  • * Solar physics and solar dynamo.
  • * Computational astrophysics and MHD modeling.

Background:

  • * Accurate solar wind modeling is crucial for space weather forecasting.
  • * Observing the Sun's full magnetic field is limited from Earth.
  • * Helioseismology offers a way to infer far-side solar activity.

Purpose of the Study:

  • * To integrate helioseismic far-side active region data into solar wind models.
  • * To assess the impact of this data on space weather forecasting accuracy.
  • * To compare a new model (FARM) with a standard model (SFTM).

Main Methods:

  • * Assimilation of far-side active regions derived from helioseismology.
  • * Comparative analysis using the Surface Flux Transport Model (SFTM) and Far-side Active Region Model (FARM).
  • * Statistical evaluation with the Wang-Sheeley-Arge (WSA) solar wind model and 3D MHD modeling with EUHFORIA.

Main Results:

  • * Including far-side magnetic data improved solar wind forecasts by up to 50% in correlation.
  • * Forecast accuracy (RMSE, MAE) improved by 3% with far-side data.
  • * 3D MHD modeling revealed significant localized differences in heliospheric structure.

Conclusions:

  • * Assimilating helioseismic far-side information enhances solar wind and space weather forecasting.
  • * Far-side data is essential for accurate modeling of heliospheric dynamics.
  • * This approach improves predictions of solar wind, transients, and geomagnetic disturbances.