Spicule (solar physics)

Short description: Jet of plasma in the Sun's chromosphere

Spicules near the solar limb. They appear as dark "hairs" above the solar surface.

In solar physics, a spicule is a dynamic jet of plasma, about 300 km diameter,[1] in the chromosphere of the Sun. They move upwards with speeds between 15 and 110 km/s from the photosphere and last a few minutes each.[1] They were discovered in 1877 by Angelo Secchi, but the physical mechanism that generates them is still debated.

## Contents

* 1 Description
* 2 Prevalence
* 3 Causes
* 4 References
* 5 Literature
* 6 External links

## Description

Spicules last for about 15 minutes;[2] at the solar limb they appear elongated (if seen on the disk, they are known as "mottles" or "fibrils"). They are usually associated with regions of high magnetic flux; their mass flux is about 100 times that of the solar wind. They rise at a rate of 20 km/s (or 72,000 km/h) and can reach several thousand kilometers in height before collapsing and fading away.

## Prevalence

There are about 3,000,000 active spicules at any one time on the Sun's chromosphere.[2] An individual spicule typically reaches 3,000–10,000 km altitude above the photosphere.[3]

## Causes

This section is missing information about numerous other proposed mechanisms. Please expand the section to include this information. Further details may exist on the talk page. (October 2019)

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Bart De Pontieu (Lockheed Martin Solar and Astrophysics Laboratory, Palo Alto, California, United States), Robert Erdélyi and Stewart James (both from the University of Sheffield, United Kingdom) hypothesised in 2004 that spicules formed as a result of P-mode oscillations in the Sun's surface, sound waves with a period of about five minutes that causes the Sun's surface to rise and fall at several hundred meters per second (see helioseismology). Magnetic flux tubes that tilted away from the vertical can focus and guide the rising material up into the solar atmosphere to form a spicule. There is still however some controversy about the issue in the solar physics community.

## References

1. ↑ 1.0 1.1 Quantifying Spicules, Tiago M. D. Pereira, Bart De Pontieu, and Mats Carlsson, The Astrophysical Journal 759, #1 (October 2012), pp. 18-34, doi:10.1088/0004-637X/759/1/18, Bibcode: 2012ApJ...759...18P.
2. ↑ 2.0 2.1 Freedman, Roger A.; Kaufmann III, William J. (2008). Universe. New York, USA: W. H. Freeman and Company. pp. 762. ISBN 978-0-7167-8584-2. https://archive.org/details/universe0008edfree.
3. ↑ §1, Two Dynamical Models for Solar Spicules, Paul Lorrain and Serge Koutchmy, Solar Physics 165, #1 (April 1996), pp. 115–137, doi:10.1007/BF00149093, Bibcode: 1996SoPh..165..115L.

## Literature

* De Pontieu, B., Erdélyi, R. and James, S: Solar chromospheric spicules from the leakage of photospheric oscillations and flows In: Nature. 430/2004, p. 536–539, ISSN 0028-0836

## External links

* NASA Astronomy Picture of the Day: Spicules: Jets on the Sun (2 November 2008)

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The Sun

Internal structure|

* Core
* Radiation zone
* Tachocline
* Convection zone

Atmosphere|

| Photosphere|

* Supergranulation
* Granule
* Faculae
* Sunspot

|

Chromosphere|

* Plage
* Spicule
* Moreton wave

Corona|

* Transition region
* Coronal hole
* Coronal loop
* Coronal mass ejection
* Prominence
* Helmet streamer
* Supra-arcade downflows

Variation|

* Solar cycle
* List of solar cycles
* Solar maximum
* Solar minimum
* Wolf number
* Solar wind
* Flare
* Helioseismology

Heliosphere|

* Current sheet
* Termination shock
* Heliosheath
* Heliopause
* Bow shock

Related|

* Heliophysics
* Solar activity
* Solar astronomy
* Solar dynamo
* Eclipse
* Solar energy
* Solar neutrino
* Solar observation
* Solar phenomena
* Solar physics
* Solar System
* Solar telescope
* Solar time
* Space climate
* Space weather
* Standard solar model
* Star
* Sunlight radiation

* Spectral class: G-type main-sequence star

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