Coronal Mass Ejections and Solar Filament Disappearances at Solar Maximum

In the present work, we will highlight the solar observation during 15th April 2012, solar filament eruption which is accompanied by an intense and gradual Coronal Mass Ejections (CMEs). The explosion of CMEs was observed at 2:12:06 UT and also can be observed by the Solar Dynamics Observatory (SDO) with an Active Region AR1458 is crackling with C-class solar flares. The solar flare class B3 and C2 were observed beginning 2241 UT and 0142 UT. The event is considered as second largest CMEs been detected since five years. Although the solar activity within a few days is considered quite low and there are no proton events were observed at geosynchronous orbit., the is still an unexpected explosion of CMEs can be occurred. The radio flux number (10.7 cm) exceeds 102 with the number of sunspot and area of sunspot increased to 77 and 270. The velocity of CMEs was calculated based on the LASCO2 data. From the results, it is clearly seen that the range of the velocity is between 200 kms-1 to 2000 kms-1. This wide of range proved that the mechanism of the CMEs is a gradual process. The explosion of CMEs velocity is located from 80º - 255º from North of the Sun. We can then conclude that currently, the rearrangement of the magnetic field, and solar flares may result in the formation of a shock that accelerates particles ahead of the CMEs loop and an active region play an important character in this event.

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Solar Eruptions - the Effects on the Earth’s Environment

Highlights of Astronomy ◽

10.1017/s1539299600013824 ◽

2002 ◽

Vol 12 ◽

pp. 384-388

Author(s):

P. Brekke

Keyword(s):

Space Weather ◽

Coronal Mass Ejections ◽

Solar Maximum ◽

Space Environment ◽

The Sun ◽

Technological Systems ◽

Heliospheric Observatory ◽

Time Space ◽

New Information ◽

Solar Eruptions

AbstractThe response of our space environment to the constantly changing Sun is known as ”Space Weather”. The Solar and Heliospheric Observatory (SOHO) has obtained significant new information about coronal mass ejections (CMEs), the source of the most severe disturbances in the Earth’s environment. Most of the time space weather is of little concern in our everyday lives. However, when the space environment is disturbed by the variable outputs of the Sun, technologies that we depend on both in orbit and on the ground can be affected. The increasing deployment of radiation-, current-, and field-sensitive technological systems over the last few decades and the increasing presence of complex systems in space combine to make society more vulnerable to solar-terrestrial disturbances. Thus, our society is much more sensitive to space weather activity today compared to the last solar maximum. By observing the Sun 24 hours per day, SOHO has proved to be an important “space weather watchdog”. The importance of real-time monitoring of the Sun will be pointed out and a number of enterprises affected by space weather will be discussed.

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The association of Coronal Mass Ejections during solar maximum times with the heliomagnetic current sheet

Advances in Space Research ◽

10.1016/0273-1177(93)90475-q ◽

1993 ◽

Vol 13 (9) ◽

pp. 183-186

Author(s):

B. Mendoza ◽

R. Pérez-Enríquez

Keyword(s):

Current Sheet ◽

Coronal Mass Ejections ◽

Solar Maximum

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Solar filament eruptions and their physical role in triggering coronal mass ejections

Advances in Space Research ◽

10.1016/j.asr.2012.12.026 ◽

2013 ◽

Vol 51 (11) ◽

pp. 1967-1980 ◽

Cited By ~ 80

Author(s):

B. Schmieder ◽

P. Démoulin ◽

G. Aulanier

Keyword(s):

Coronal Mass Ejections ◽

Physical Role ◽

Solar Filament

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GONG Catalog of Solar Filament Oscillations Near Solar Maximum

The Astrophysical Journal Supplement Series ◽

10.3847/1538-4365/aabde7 ◽

2018 ◽

Vol 236 (2) ◽

pp. 35 ◽

Cited By ~ 16

Author(s):

M. Luna ◽

J. Karpen ◽

J. L. Ballester ◽

K. Muglach ◽

J. Terradas ◽

...

Keyword(s):

Solar Maximum ◽

Solar Filament

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Probable detection of an eruptive filament from a superflare on a solar-type star

Nature Astronomy ◽

10.1038/s41550-021-01532-8 ◽

2021 ◽

Author(s):

Kosuke Namekata ◽

Hiroyuki Maehara ◽

Satoshi Honda ◽

Yuta Notsu ◽

Soshi Okamoto ◽

...

Keyword(s):

Coronal Mass Ejection ◽

Coronal Mass Ejections ◽

Spectroscopic Observation ◽

Type Star ◽

Filament Eruption ◽

Radiated Energy ◽

Solar Type ◽

Solar Filament ◽

Mass Ejection ◽

Solar Type Star

AbstractSolar flares are often accompanied by filament/prominence eruptions (~104 K and ~1010−11 cm−3), sometimes leading to coronal mass ejections that directly affect the Earth’s environment1,2. ‘Superflares’ are found on some active solar-type (G-type main-sequence) stars3–5, but the filament eruption–coronal mass ejection association has not been established. Here we show that our optical spectroscopic observation of the young solar-type star EK Draconis reveals evidence for a stellar filament eruption associated with a superflare. This superflare emitted a radiated energy of 2.0 × 1033 erg, and a blueshifted hydrogen absorption component with a high velocity of −510 km s−1 was observed shortly afterwards. The temporal changes in the spectra strongly resemble those of solar filament eruptions. Comparing this eruption with solar filament eruptions in terms of the length scale and velocity strongly suggests that a stellar coronal mass ejection occurred. The erupted filament mass of 1.1 × 1018 g is ten times larger than those of the largest solar coronal mass ejections. The massive filament eruption and an associated coronal mass ejection provide the opportunity to evaluate how they affect the environment of young exoplanets/the young Earth6 and stellar mass/angular momentum evolution7.

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Coronal mass ejections observed during the Solar Maximum Mission: Latitude distribution and rate of occurrence

Journal of Geophysical Research Atmospheres ◽

10.1029/ja089ia05p02639 ◽

1984 ◽

Vol 89 (A5) ◽

pp. 2639 ◽

Cited By ~ 128

Author(s):

A. J. Hundhausen ◽

C. B. Sawyer ◽

L. House ◽

R. M. E. Illing ◽

W. J. Wagner

Keyword(s):

Coronal Mass Ejections ◽

Solar Maximum ◽

Solar Maximum Mission ◽

Latitude Distribution

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Observations of radio spectra at 1–2.5 GHz associated with CME start time

Proceedings of the International Astronomical Union ◽

10.1017/s1743921309029482 ◽

2008 ◽

Vol 4 (S257) ◽

pp. 317-321

Author(s):

José R. Cecatto

Keyword(s):

Radio Emission ◽

Coronal Mass Ejections ◽

Solar Radio ◽

Solar Maximum ◽

Radio Spectrum ◽

The Sun ◽

Radio Bursts ◽

Start Time ◽

Trigger Mechanism ◽

Made In

AbstractWe know Coronal Mass Ejections (CME) and flares are the most energetic phenomena happening on the Sun. Until now the information about origin and trigger mechanism of CMEs remains scarce. Also, there is unconclusive information about the association between them and flares although progress has been made in recent years. Multi-spectral observations suggested that the flare energy release occurs in regions from where the decimetric radio emission originates. In this case, investigations of the solar emission in this wavelength range can give us valuable information about these questions. During last solar maximum the Brazilian Solar Spectroscope (BSS) observed the solar radio spectrum (1–2.5 GHz) with high time (100–20 ms) and frequency (50–100 channels) resolutions on a daily (11–19 UT) basis. A survey during the period 1999–2002, shows that a significant fraction (20% –57 events) of CMEs recorded by LASCO has an association with the spectra of radio bursts recorded by BSS. Analysis of the radio spectrum associated to CME shows there is a dominance of continuum and/or pulsation and that the association becomes stronger when we consider the CME acceleration since its origin on the Sun. A statistics of this association between CME dynamics and the characteristics of decimetric radio bursts recorded by BSS is presented. Emphasis is given to observations of the association with CME start time.

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