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 Field Lines01:19

Magnetic Field Lines

4.0K
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:
4.0K
Magnetic Field of a Solenoid01:18

Magnetic Field of a Solenoid

3.7K
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...
3.7K
Magnetostatic Boundary Conditions01:28

Magnetostatic Boundary Conditions

838
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...
838
Magnetic Flux01:18

Magnetic Flux

3.4K
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...
3.4K
Magnetic Field Of A Current Loop01:16

Magnetic Field Of A Current Loop

4.3K
Consider a circular loop with a radius a, that carries a current I. The magnetic field due to the current at an arbitrary point P along the axis of the loop can be calculated using the Biot-Savart law.
4.3K
General External Flow Characteristics01:26

General External Flow Characteristics

57
The study of external flow is essential for creating structures and objects that interact efficiently and safely with moving fluids, such as air or water. When a body is immersed in a flowing fluid, it experiences two primary forces: drag, which opposes motion along the flow direction, and lift, which acts perpendicular to the flow. The shape, size, and orientation of the object influence these forces.Streamlined and Blunt Bodies in External FlowObjects in fluid flow are classified as...
57

You might also read

Related Articles

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

Sort by
Same authorSame journal

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

Solar physics·2026
Same authorSame journal

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

Solar physics·2026
Same author

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

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

Multi-source connectivity as the driver of solar wind variability in the heliosphere.

Nature astronomy·2024
Same author

Picoflare jets power the solar wind emerging from a coronal hole on the Sun.

Science (New York, N.Y.)·2023
Same author

Defining the Middle Corona.

Solar physics·2023
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
Same journal

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

Solar physics·2026
See all related articles

Related Experiment Video

Updated: May 15, 2025

X-ray Beam Induced Current Measurements for Multi-Modal X-ray Microscopy of Solar Cells
00:10

X-ray Beam Induced Current Measurements for Multi-Modal X-ray Microscopy of Solar Cells

Published on: August 20, 2019

13.7K

Investigating Solar Wind Outflows from Open-Closed Magnetic Field Structures Using Coordinated Solar Orbiter and

Nawin Ngampoopun1, Roberto Susino2, David H Brooks3,1

  • 1Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey, RH5 6NT UK.

Solar Physics
|April 7, 2025
PubMed
Summary
This summary is machine-generated.

Investigating solar wind outflows from ESA/NASA

More Related Videos

Investigation of Early Plasma Evolution Induced by Ultrashort Laser Pulses
11:20

Investigation of Early Plasma Evolution Induced by Ultrashort Laser Pulses

Published on: July 2, 2012

14.9K
Spectral and Angle-Resolved Magneto-Optical Characterization of Photonic Nanostructures
08:01

Spectral and Angle-Resolved Magneto-Optical Characterization of Photonic Nanostructures

Published on: November 21, 2019

7.0K

Related Experiment Videos

Last Updated: May 15, 2025

X-ray Beam Induced Current Measurements for Multi-Modal X-ray Microscopy of Solar Cells
00:10

X-ray Beam Induced Current Measurements for Multi-Modal X-ray Microscopy of Solar Cells

Published on: August 20, 2019

13.7K
Investigation of Early Plasma Evolution Induced by Ultrashort Laser Pulses
11:20

Investigation of Early Plasma Evolution Induced by Ultrashort Laser Pulses

Published on: July 2, 2012

14.9K
Spectral and Angle-Resolved Magneto-Optical Characterization of Photonic Nanostructures
08:01

Spectral and Angle-Resolved Magneto-Optical Characterization of Photonic Nanostructures

Published on: November 21, 2019

7.0K

Area of Science:

  • Solar Physics
  • Plasma Physics
  • Astrophysics

Background:

  • The solar corona is the source of the solar wind.
  • Understanding solar wind origins requires close-up observations and multi-perspective views.
  • The Solar Orbiter (SO) mission provides unprecedented data for studying the corona.

Purpose of the Study:

  • To analyze and compare solar wind outflows from a narrow open-field corridor and a mid-latitude coronal hole.
  • To investigate the relationship between plasma properties and magnetic field structures in the solar corona.
  • To understand the drivers of solar wind variability.

Main Methods:

  • Observations by the Metis coronagraph (SO) and the Extreme Ultraviolet Imaging Spectrometer (EIS) (Hinode).
  • Analysis of solar wind outflows from off-limb and on-disk observations.
  • Magnetic field extrapolations to identify source regions.

Main Results:

  • Plasma from the open-field corridor showed higher electron densities and lower outflow velocities than coronal hole plasma in the middle corona.
  • Source regions in the low corona exhibited similar plasma properties.
  • Solar wind speed from the open-field corridor did not correlate with the magnetic field expansion factor, unlike the coronal hole.

Conclusions:

  • Differences in plasma properties at higher altitudes suggest dynamic processes in the low-middle corona.
  • Magnetic reconnection may play a significant role in driving solar wind variability.
  • The origin of the solar wind is complex and depends on specific coronal structures and dynamics.