Generation of solar spicules and subsequent atmospheric heating

Tanmoy Samanta; Hui Tian; Vasyl Yurchyshyn; Hardi Peter; Wenda Cao; Alphonse Sterling; Robertus Erdélyi; Kwangsu Ahn; Song Feng; Dominik Utz; Dipankar Banerjee; Yajie Chen

doi:10.1126/science.aaw2796

Generation of solar spicules and subsequent atmospheric heating

Tanmoy Samanta, Hui Tian, Vasyl Yurchyshyn, Hardi Peter, Wenda Cao, Alphonse Sterling, Robertus Erdélyi, Kwangsu Ahn, Song Feng, Dominik Utz, Dipankar Banerjee, Yajie Chen

Center For Solar Terrestrial Research - Big Bear Solar Observatory

Research output: Contribution to journal › Article › peer-review

114 Scopus citations

Abstract

Spicules are rapidly evolving fine-scale jets of magnetized plasma in the solar chromosphere. It remains unclear how these prevalent jets originate from the solar surface and what role they play in heating the solar atmosphere. Using the Goode Solar Telescope at the Big Bear Solar Observatory, we observed spicules emerging within minutes of the appearance of opposite-polarity magnetic flux around dominant-polarity magnetic field concentrations. Data from the Solar Dynamics Observatory showed subsequent heating of the adjacent corona. The dynamic interaction of magnetic fields (likely due to magnetic reconnection) in the partially ionized lower solar atmosphere appears to generate these spicules and heat the upper solar atmosphere.

Original language	English (US)
Pages (from-to)	890-894
Number of pages	5
Journal	Science
Volume	366
Issue number	6467
DOIs	https://doi.org/10.1126/science.aaw2796
State	Published - Nov 15 2019

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title = "Generation of solar spicules and subsequent atmospheric heating",

abstract = "Spicules are rapidly evolving fine-scale jets of magnetized plasma in the solar chromosphere. It remains unclear how these prevalent jets originate from the solar surface and what role they play in heating the solar atmosphere. Using the Goode Solar Telescope at the Big Bear Solar Observatory, we observed spicules emerging within minutes of the appearance of opposite-polarity magnetic flux around dominant-polarity magnetic field concentrations. Data from the Solar Dynamics Observatory showed subsequent heating of the adjacent corona. The dynamic interaction of magnetic fields (likely due to magnetic reconnection) in the partially ionized lower solar atmosphere appears to generate these spicules and heat the upper solar atmosphere.",

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doi = "10.1126/science.aaw2796",

language = "English (US)",

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TY - JOUR

T1 - Generation of solar spicules and subsequent atmospheric heating

AU - Samanta, Tanmoy

AU - Tian, Hui

AU - Yurchyshyn, Vasyl

AU - Peter, Hardi

AU - Cao, Wenda

AU - Sterling, Alphonse

AU - Erdélyi, Robertus

AU - Ahn, Kwangsu

AU - Feng, Song

AU - Utz, Dominik

AU - Banerjee, Dipankar

AU - Chen, Yajie

PY - 2019/11/15

Y1 - 2019/11/15

N2 - Spicules are rapidly evolving fine-scale jets of magnetized plasma in the solar chromosphere. It remains unclear how these prevalent jets originate from the solar surface and what role they play in heating the solar atmosphere. Using the Goode Solar Telescope at the Big Bear Solar Observatory, we observed spicules emerging within minutes of the appearance of opposite-polarity magnetic flux around dominant-polarity magnetic field concentrations. Data from the Solar Dynamics Observatory showed subsequent heating of the adjacent corona. The dynamic interaction of magnetic fields (likely due to magnetic reconnection) in the partially ionized lower solar atmosphere appears to generate these spicules and heat the upper solar atmosphere.

AB - Spicules are rapidly evolving fine-scale jets of magnetized plasma in the solar chromosphere. It remains unclear how these prevalent jets originate from the solar surface and what role they play in heating the solar atmosphere. Using the Goode Solar Telescope at the Big Bear Solar Observatory, we observed spicules emerging within minutes of the appearance of opposite-polarity magnetic flux around dominant-polarity magnetic field concentrations. Data from the Solar Dynamics Observatory showed subsequent heating of the adjacent corona. The dynamic interaction of magnetic fields (likely due to magnetic reconnection) in the partially ionized lower solar atmosphere appears to generate these spicules and heat the upper solar atmosphere.

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Generation of solar spicules and subsequent atmospheric heating

Abstract

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