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A coronal hole is a temporary region of relatively cool, less dense plasma in the solar corona where the Sun's magnetic field extends into interplanetary space as an open field. Compared to the corona's usual closed magnetic field that arches between regions of opposite magnetic polarity, the open magnetic field of a coronal hole allows solar wind to escape into space at a much quicker rate. This results in decreased temperature and density of the plasma at the site of a coronal hole, as well as an increased speed in the average solar wind measured in interplanetary space. If streams of high-speed solar wind from coronal holes encounter the Earth, they can cause major displays of aurorae. Near solar minimum, when activity such as coronal mass ejections is less frequent, such streams are the main cause of geomagnetic storms and associated aurorae.

History
In the 1960s, coronal holes showed up on X-ray images taken by sounding rockets and in observations at radio wavelengths by the Sydney Chris Cross radio telescope, but at the time, what they were was unclear. Their true nature was recognized in the 1970s, when X-ray telescopes in the Skylab mission were flown above the Earth's atmosphere to reveal the structure of the corona.

Solar cycle

Coronal hole size and population correspond with the solar cycle. As the Sun heads toward solar maximum, the coronal holes move closer and closer to the Sun's poles. During solar maxima, the number of coronal holes decreases until the magnetic fields on the Sun reverse. Afterwards, new coronal holes appear near the new poles. The coronal holes then increase in size and number, extending farther from the poles as the Sun moves toward a solar minimum again.

Solar wind

Coronal holes generally discharge solar wind at a speed about twice the average. The escaping solar wind is known to travel along open magnetic field lines that pass through the coronal hole area. Since coronal holes are regions in the Sun's corona that have much lower densities and temperatures than most of the corona, these regions are very thin, which contributes to the solar wind, since particles within the chromosphere can more easily break through.

Influence on space weather
During solar minima, coronal holes are the primary sources of space weather disturbances, including aurorae. Typically, geomagnetic (and proton) storms originating from coronal holes have a gradual commencement (over hours) and are not as severe as storms caused by coronal mass ejections (CMEs), which usually have a sudden onset. Because coronal holes can last for several solar rotations (i.e. several months), predicting the recurrence of this type of disturbance is often possible significantly farther in advance than for CME-related disturbances.

See also
Heliophysics
List of solar storms

References

Further reading

Jiang, Y., Chen, H., Shen, Y., Yang, L., & Li, K. (2007, January). Hα dimming associated with the eruption of a coronal sigmoid in the quiet Sun. Solar Physics, 240(1), 77–87.

Solar phenomena
Anthrax xanthomeros är en tvåvingeart som beskrevs av Marston 1970. Anthrax xanthomeros ingår i släktet Anthrax och familjen svävflugor.

Artens utbredningsområde är Belize. Inga underarter finns listade i Catalogue of Life.

Källor

Svävflugor
xanthomeros
Ablabesmyia variipes är en tvåvingeart som först beskrevs av Jean-Jacques Kieffer 1910. Ablabesmyia variipes ingår i släktet Ablabesmyia och familjen fjädermyggor.

Artens utbredningsområde är Burma. Inga underarter finns listade i Catalogue of Life.

Källor

Fjädermyggor
variipes
Fimbulheimen is a mountain range in Queen Maud Land, Antarctica. It stretches from Jutulstraumen by 1° west of Carsten Borchgrevink Ice at 18° east, about 200 km from the ice edge. Fimbulheimen is thus between Maudheim Plateau and Sør-Rondane.

Dronning Maud's highest mountain, Jøkulkyrkja (elevation 3148 m), is located in Mühlig-Hofmann Mountains in Fimbulheimen. The name comes from Fimbulvetr, the harsh winter immediately preceding Ragnarok in Norse mythology.

A number of smaller ranges and mountain areas constitutes Fimbulheimen, from west to east:
Gburek Peaks
Sverdrup Mountains
Gjelsvik Mountains
Mühlig-Hofmann Mountains
Orvin Mountains
Filchner Mountains
Drygalski Mountains
Kurze Mountains
Gagarin Mountains
Conrad Mountains
Mount Dallmann
Wohlthat Mountains
Humboldt Mountains
Petermann Ranges
Gruber Mountains
Hoel Mountains
Weyprecht Mountains
Payer Mountains
Lomonosov Mountains


The Norwegian research station Troll is located by Jutulsessen Mountain west in Fimbulheimen, while the ornithological field station Tor is about 100 km further east at Svarthamaren Mountain in Mühlig-Hofmann Mountains.

Large parts of the area were mapped by the Norwegian Antarctic Expedition 1956-60. The Norwegian Polar Institute has published twelve map sheets of Fimbulheimen in scale 1:250 000.

References

Mountain ranges of Queen Maud Land
Princess Astrid Coast
Gorazd Andrejč, slovenski filozof, religiolog in teolog

Končal je študij filozofije na Univerzi v Mariboru, magistriral iz judovsko-krščanskih odnosov (interdisciplinarni študij) na Univerzi v Cambridgu, ter doktoriral iz področja filozofije religije na Univerzi v Exeterju v Veliki Britaniji.

Je predavatelj na Univerzi v Groningenu na Nizozemskem ter raziskovalec na Inštitutu za filozofske študije na Znanstveno-raziskovalnem središču Koper.

Bibliografija

Religijski pojmovnik za mlade (Aristej, 2018)
Wittgenstein and Interreligious Disagreement (Palgrave Macmillan, 2016)
Interpreting Interreligious Relations with Wittgenstein: Philosophy, Theology and Religious Studies (Brill, 2019)

Neznano leto rojstva (živeči ljudje)
Živeči ljudje
Slovenski filozofi
Slovenski teologi
Diplomiranci Filozofske fakultete v Mariboru
Magistrirali na Univerzi v Cambridgeu
Doktorirali na Univerzi v Exetru
Predavatelji na Univerzi v Groningenu
Andrejč, Gorazd
Agapetes auriculata är en ljungväxtart som beskrevs av George Bentham och Hook. f. Agapetes auriculata ingår i släktet Agapetes och familjen ljungväxter. Inga underarter finns listade i Catalogue of Life.

Cartiere din Brașov

A coronal hole is a temporary region of relatively cool, less dense plasma in the solar corona where the Sun's magnetic field extends into interplanetary space as an open field. Compared to the corona's usual closed magnetic field that arches between regions of opposite magnetic polarity, the open magnetic field of a coronal hole allows solar wind to escape into space at a much quicker rate. This results in decreased temperature and density of the plasma at the site of a coronal hole, as well as an increased speed in the average solar wind measured in interplanetary space. If streams of high-speed solar wind from coronal holes encounter the Earth, they can cause major displays of aurorae. Near solar minimum, when activity such as coronal mass ejections is less frequent, such streams are the main cause of geomagnetic storms and associated aurorae.

History

In the 1960s, coronal holes showed up on X-ray images taken by sounding rockets and in observations at radio wavelengths by the Sydney Chris Cross radio telescope, but at the time, what they were was unclear. Their true nature was recognized in the 1970s, when X-ray telescopes in the Skylab mission were flown above the Earth's atmosphere to reveal the structure of the corona.

Solar cycle

Coronal hole size and population correspond with the solar cycle. As the Sun heads toward solar maximum, the coronal holes move closer and closer to the Sun's poles. During solar maxima, the number of coronal holes decreases until the magnetic fields on the Sun reverse. Afterwards, new coronal holes appear near the new poles. The coronal holes then increase in size and number, extending farther from the poles as the Sun moves toward a solar minimum again.

Solar wind

Coronal holes generally discharge solar wind at a speed about twice the average. The escaping solar wind is known to travel along open magnetic field lines that pass through the coronal hole area. Since coronal holes are regions in the Sun's corona that have much lower densities and temperatures than most of the corona, these regions are very thin, which contributes to the solar wind, since particles within the chromosphere can more easily break through.

Influence on space weather

During solar minima, coronal holes are the primary sources of space weather disturbances, including aurorae. Typically, geomagnetic (and proton) storms originating from coronal holes have a gradual commencement (over hours) and are not as severe as storms caused by coronal mass ejections (CMEs), which usually have a sudden onset. Because coronal holes can last for several solar rotations (i.e. several months), predicting the recurrence of this type of disturbance is often possible significantly farther in advance than for CME-related disturbances.