Coronal mass ejection

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Coronal mass ejections are usually visible in white-light coronagraphs.
Part of a series of articles about
Heliophysics
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Heliospheric current sheet
Fundamentals
Interplanetary medium
Magnetospherics
Solar phenomena

A coronal mass ejection (CME) is a significant ejection of

solar activity
, but a broadly accepted theoretical understanding of these relationships has not been established.

If a CME enters

solar storm of 1859. Also known as the Carrington Event, it disabled parts of the newly created United States telegraph
network, starting fires and shocking some telegraph operators.

Near solar maxima, the Sun produces about three CMEs every day, whereas near solar minima, there is about one CME every five days.

Physical description

CMEs release large quantities of matter and magnetic flux from the Sun's atmosphere into the

interplanetary space. The ejected matter is a plasma consisting primarily of electrons and protons embedded within the ejected magnetic field. This magnetic field is commonly in the form of a flux rope, a helical magnetic field with changing pitch angles
.

The average mass ejected is 1.6×1012 kg (3.5×1012 lb). However, the estimated mass values for CMEs are only lower limits, because coronagraph measurements provide only two-dimensional data.

CMEs erupt from strongly twisted or sheared, large-scale magnetic field structures in the corona that are kept in equilibrium by overlying magnetic fields.

Origin

Simplified model of magnetic fields emerging from the photosphere

CMEs erupt from the lower corona, where processes associated with the local magnetic field dominate over other processes. As a result, the coronal magnetic field plays an important role in the formation and eruption of CMEs. Pre-eruption structures originate from magnetic fields that are initially generated in the Sun's interior by the solar dynamo. These magnetic fields rise to the Sun's surface—the photosphere—where they may form localized areas of highly concentrated magnetic flux and expand into the lower solar atmosphere forming active regions. At the photosphere, active region magnetic flux is often distributed in a dipole configuration, that is, with two adjacent areas of opposite magnetic polarity across which the magnetic field arches. Over time, the concentrated magnetic flux cancels and disperses across the Sun's surface, merging with the remnants of past active regions to become a part of the quiet Sun. Pre-eruption CME structures can be present at different stages of the growth and decay of these regions, but they always lie above polarity inversion lines (PIL), or boundaries across which the sign of the vertical component of the magnetic field reverses. PILs may exist in, around, and between active regions or form in the quiet Sun between active region remnants. More complex magnetic flux configurations, such as quadrupolar fields, can also host pre-eruption structures.[1][2]

In order for pre-eruption CME structures to develop, large amounts of energy must be stored and be readily available to be released. As a result of the dominance of magnetic field processes in the lower corona, the majority of the energy must be stored as magnetic energy. The magnetic energy that is freely available to be released from a pre-eruption structure, referred to as the magnetic free energy or nonpotential energy of the structure, is the excess magnetic energy stored by the structure's magnetic configuration relative to that stored by the lowest-energy magnetic configuration the underlying photospheric magnetic flux distribution could theoretically take, a potential field state. Emerging magnetic flux and photospheric motions continuously shifting the footpoints of a structure can result in magnetic free energy building up in the coronal magnetic field as twist or shear.[3] Some pre-eruption structures, referred to as sigmoids, take on an S or reverse-S shape as shear accumulates. This has been observed in active region coronal loops and filaments with forward-S sigmoids more common in the southern hemisphere and reverse-S sigmoids more common in the northern hemisphere.[4][5]

Magnetic flux ropes—twisted and sheared

magnetic flux tubes that can carry electric current and magnetic free energy—are an integral part of the post-eruption CME structure; however, whether flux ropes are always present in the pre-eruption structure or whether they are created during the eruption from a strongly sheared core field (see § Initiation) is subject to ongoing debate.[3][6]

Some pre-eruption structures have been observed to support prominences, also known as filaments, composed of much cooler material than the surrounding coronal plasma. Prominences are embedded in magnetic field structures referred to as prominence cavities, or filament channels, which may constitute part of a pre-eruption structure (see § Coronal signatures).

Early evolution

The early evolution of a CME involves its initiation from a pre-eruption structure in the corona and the acceleration that follows. The processes involved in the early evolution of CMEs are poorly understood due to a lack of observational evidence.

Initiation

CME initiation occurs when a pre-eruption structure in an equilibrium state enters a nonequilibrium or

metastable state where energy can be released to drive an eruption. The specific processes involved in CME initiation are debated, and various models have been proposed to explain this phenomenon based on physical speculation. Furthermore, different CMEs may be initiated by different processes.[6]: 175 [7]
: 303 

It is unknown whether a magnetic flux rope exists prior to initiation, in which case either ideal or non-ideal magnetohydrodynamic (MHD) processes drive the expulsion of this flux rope, or whether a flux rope is created during the eruption by non-ideal process.[8][9]: 555  Under ideal MHD, initiation may involve ideal instabilities or catastrophic loss of equilibrium along an existing flux rope:[3]

  • The kink instability occurs when a magnetic flux rope is twisted to a critical point, whereupon the flux rope is unstable to further twisting.
  • The torus instability occurs when the magnetic field strength of an arcade overlying a flux rope decreases rapidly with height. When this decrease is sufficiently rapid, the flux rope is unstable to further expansion.[10]
  • The catastrophe model involves a catastrophic loss of equilibrium.

Under non-ideal MHD, initiations mechanisms may involve resistive instabilities or magnetic reconnection:

  • Tether-cutting, or flux cancellation, occurs in strongly sheared arcades when nearly antiparallel field lines on opposite sides of the arcade form a current sheet and reconnect with each other. This can form a helical flux rope or cause a flux rope already present to grow and its axis to rise.
  • The magnetic breakout model consists of an initial quadrupolar magnetic topology with a null point above a central flux system. As shearing motions cause this central flux system to rise, the null point forms a current sheet and the core flux system reconnects with overlying magnetic field.[9]
Video of a solar filament being launched

Initial acceleration

Following initiation, CMEs are subject to different forces that either assist or inhibit their rise through the lower corona. Downward magnetic tension force exerted by the strapping magnetic field as it is stretched and, to a lesser extent, the gravitational pull of the Sun oppose movement of the core CME structure. In order for sufficient acceleration to be provided, past models have involved magnetic reconnection below the core field or an ideal MHD process, such as instability or acceleration from the solar wind.

In the majority of CME events, acceleration is provided by magnetic reconnection cutting the strapping field's connections to the photosphere from below the core and outflow from this reconnection pushing the core upward. When the initial rise occurs, the opposite sides of the strapping field below the rising core are oriented nearly

positive feedback loop results as the core is pushed upwards and the sides of the strapping field are brought in closer and closer contact to produce additional magnetic reconnection and rise. While upward reconnection outflow accelerates the core, simultaneous downward outflow is sometimes responsible for other phenomena associated with CMEs (see § Coronal signatures
).

In cases where significant magnetic reconnection does not occur, ideal MHD instabilities or the dragging force from the solar wind can theoretically accelerate a CME. However, if sufficient acceleration is not provided, the CME structure may fall back in what is referred to as a failed or confined eruption.[9][3]

Coronal signatures

The early evolution of CMEs is frequently associated with other solar phenomena observed in the low corona, such as eruptive prominences and solar flares. CMEs that have no observed signatures are sometimes referred to as stealth CMEs.[11][12]

Prominences embedded in some CME pre-eruption structures may erupt with the CME as eruptive prominences. Eruptive prominences are associated with at least 70% of all CMEs[13] and are often embedded within the bases of CME flux ropes. When observed in white-light coronagraphs, the eruptive prominence material, if present, corresponds to the observed bright core of dense material.[7]

When magnetic reconnection is excited along a current sheet of a rising CME core structure, the downward reconnection outflows can collide with loops below to form a cusp-shaped, two-ribbon solar flare.

CME eruptions can also produce EUV waves, also known as EIT waves after the Extreme ultraviolet Imaging Telescope or as Moreton waves when observed in the chromosphere, which are fast-mode MHD wave fronts that emanate from the site of the CME.[6][3]

A coronal dimming is a localized decrease in

soft X-ray emissions in the lower corona. When associated with a CME, coronal dimmings are thought to occur predominantly due to a decrease in plasma density caused by mass outflows during the expansion of the associated CME. They often occur either in pairs located within regions of opposite magnetic polarity, a core dimming, or in a more widespread area, a secondary dimming. Core dimmings are interpreted as the footpoint locations of the erupting flux rope; secondary dimmings are interpreted as the result of the expansion of the overall CME structure and are generally more diffuse and shallow.[14] Coronal dimming was first reported in 1974,[15] and, due to their appearance resembling that of coronal holes, they were sometimes referred to as transient coronal holes.[16]

Propagation

Observations of CMEs are typically through white-light coronagraphs which measure the Thomson scattering of sunlight off of free electrons within the CME plasma.[17] An observed CME may have any or all of three distinctive features: a bright core, a dark surrounding cavity, and a bright leading edge.[18] The bright core is usually interpreted as a prominence embedded in the CME (see § Origin) with the leading edge as an area of compressed plasma ahead of the CME flux rope. However, some CMEs exhibit more complex geometry.[7]

From white-light coronagraph observations, CMEs have been measured to reach speeds in the plane-of-sky ranging from 20 to 3,200 km/s (12 to 2,000 mi/s) with an average speed of 489 km/s (304 mi/s) 1996 and 2003.[19] Observations of CME speeds indicate that CMEs tend to accelerate or decelerate until they reach the speed of the solar wind (§ Interactions in the heliosphere).

When observed in interplanetary space at distances greater than about 50 solar radii (0.23 AU) away from the Sun, CMEs are sometimes referred to as interplanetary CMEs, or ICMEs.[6]: 4 

Interactions in the heliosphere

As CMEs propagate through the heliosphere, they may interact with the surrounding solar wind, the interplanetary magnetic field, and other CMEs and celestial bodies.

CMEs can experience aerodynamic drag forces that act to bring them to kinematic equilibrium with the solar wind. As a consequence, CMEs faster than the solar wind tend to slow down whereas CMEs slower than the solar wind tend to speed up until their speed matches that of the solar wind.[20]

How CMEs evolve as they propagate through the heliosphere is poorly understood. Models of their evolution have been proposed that are accurate to some CMEs but not others. Aerodynamic drag and snowplow models assume that ICME evolution is governed by its interactions with the solar wind. Aerodynamic drag alone may be able to account for the evolution of some ICMEs, but not all of them.[6]: 199 

Follow a CME as it passes Venus then Earth, and explore how the Sun drives Earth's winds and oceans

CMEs typically reach Earth one to five days after leaving the Sun. The strongest deceleration or acceleration occurs close to the Sun, but it can continue even beyond Earth orbit (1 AU), which was observed using measurements at Mars[21] and by the Ulysses spacecraft.[22] ICMEs faster than about 500 km/s (310 mi/s) eventually drive a shock wave.[23] This happens when the speed of the ICME in the frame of reference moving with the solar wind is faster than the local fast magnetosonic speed. Such shocks have been observed directly by coronagraphs[24] in the corona, and are related to type II radio bursts. They are thought to form sometimes as low as 2 R☉ (solar radii). They are also closely linked with the acceleration of solar energetic particles.[25]

As ICMEs propagate through the interplanetary medium, they may collide with other ICMEs in what is referred to as CME–CME interaction or CME cannibalism.[9]: 599 

During such CME-CME interactions, the first CME may clear the way for the second one[26][27][28] and/or when two CMEs collide[29][30] it can lead to more severe impacts on Earth. Historical records show that the most extreme space weather events involved multiple successive CMEs. For example, the famous Carrington event in 1859 had several eruptions and caused auroras to be visible at low latitudes for four nights.[31] Similarly, the solar storm of September 1770 lasted for nearly nine days and also caused repeated low-latitude auroras.[32] The interaction between two moderate CMEs between the Sun and Earth can create extreme conditions on Earth. Recent studies have shown that the magnetic structure in particular its chirality/handedness, of a CME can greatly affect how it interacts with Earth's magnetic field. This interaction can result in the conservation or loss of magnetic flux, particularly its southward magnetic field component, through magnetic reconnection with the interplanetary magnetic field.[33]

Morphology

In the solar wind, CMEs manifest as magnetic clouds. They have been defined as regions of enhanced magnetic field strength, smooth rotation of the magnetic field vector, and low

Helios-1 two days after being observed by SMM.[35] However, because observations near Earth are usually done by a single spacecraft, many CMEs are not seen as being associated with magnetic clouds. The typical structure observed for a fast CME by a satellite such as ACE is a fast-mode shock wave
followed by a dense (and hot) sheath of plasma (the downstream region of the shock) and a magnetic cloud.

Other signatures of magnetic clouds are now used in addition to the one described above: among other, bidirectional superthermal electrons, unusual charge state or abundance of iron, helium, carbon, and/or oxygen.

The typical time for a magnetic cloud to move past a satellite at the

AU with a typical speed of 450 km/s (280 mi/s) and magnetic field strength of 20 nT.[36]

Solar cycle

Further information: Solar cycle

The frequency of ejections depends on the phase of the solar cycle: from about 0.2 per day near the solar minimum to 3.5 per day near the solar maximum.[37] However, the peak CME occurrence rate is often 6–12 months after sunspot number reaches its maximum.[3]

Impact on Earth

aurora australis
during a geomagnetic storm on 29 May 2010. The storm was most likely caused by a CME that had erupted from the Sun on 24 May 2010, five days prior to the storm.
This video features two model runs. One looks at a moderate CME from 2006. The second run examines the consequences of a large CME such as the Carrington-class CME of 1859.

Only a very small fraction of CMEs are directed toward, and reach, the Earth. A CME arriving at Earth results in a

upper atmosphere.[citation needed] This can result in events such as the March 1989 geomagnetic storm
.

CMEs, along with

electrical transmission line facilities, resulting in potentially massive and long-lasting power outages.[38][39]

Shocks in the upper corona driven by CMEs can also accelerate

solar energetic particles toward the Earth resulting in gradual solar particle events. Interactions between these energetic particles and the Earth can cause an increase in the number of free electrons in the ionosphere, especially in the high-latitude polar regions, enhancing radio wave absorption, especially within the D-region of the ionosphere, leading to polar cap absorption events.[40]

The interaction of CMEs with the Earth's

plasma waves.[42]

Halo coronal mass ejections

A halo coronal mass ejection is a CME which appears in white-light coronagraph observations as an expanding ring completely surrounding the occulting disk of the coronagraph. Halo CMEs are interpreted as CMEs directed toward or away from the observing coronagraph. When the expanding ring does not completely surround the occulting disk, but has an

angular width of more than 120 degrees around the disk, the CME is referred to as a partial halo coronal mass ejection. Partial and full halo CMEs have been found to make up about 10% of all CMEs with about 4% of all CMEs being full halo CMEs.[43] Frontside, or Earth-direct, halo CMEs are often associated with Earth-impacting CMEs; however, not all frontside halo CMEs impact Earth.[44]

Future risk

In 2019, researchers used an alternative method (Weibull distribution) and estimated the chance of Earth being hit by a Carrington-class storm in the next decade to be between 0.46% and 1.88%.[45]

History

Further information: Solar observation

First traces

CMEs have been observed indirectly for thousands of years via aurora. Other indirect observations that predated the discovery of CMEs were through measurements of geomagnetic perturbations, radioheliograph measurements of solar radio bursts, and in-situ measurements of interplanetary shocks.[6]

The largest recorded geomagnetic perturbation, resulting presumably from a CME, coincided with the first-observed

soft X-rays. This could not easily be understood at the time because it predated the discovery of X-rays in 1895 and the recognition of the ionosphere
in 1902.

About 18 hours after the flare, further geomagnetic perturbations were recorded by multiple magnetometers as a part of a geomagnetic storm. The storm disabled parts of the recently created US telegraph network, starting fires and shocking some telegraph operators.[39]

First optical observations

The first optical observation of a CME was made on 14 December 1971 using the coronagraph of

solar eclipses
are now understood as essentially the same thing.

Instruments

On 1 November 1994,

MeV energies, electromagnetic radiation from DC to 13 MHz radio waves, and gamma-rays.[citation needed
]

On 25 October 2006, NASA launched

stereoscopic images of CMEs and other solar activity measurements. The spacecraft orbit the Sun at distances similar to that of Earth, with one slightly ahead of Earth and the other trailing. Their separation gradually increased so that after four years they were almost diametrically opposite each other in orbit.[48][49]

Notable coronal mass ejections

Further information: List of solar storms

On 9 March 1989, a CME occurred, which struck Earth four days later on 13 March. It caused power failures in Quebec, Canada and short-wave radio interference.

On 23 July 2012, a massive, and potentially damaging,

Carrington-class
event.

On 14 October 2014, an ICME was photographed by the Sun-watching spacecraft

Mars Odyssey, and Mars Science Laboratory missions. On 22 October, at 3.1 AU, it reached comet 67P/Churyumov–Gerasimenko, perfectly aligned with the Sun and Mars, and was observed by Rosetta. On 12 November, at 9.9 AU, it was observed by Cassini at Saturn. The New Horizons spacecraft was at 31.6 AU approaching Pluto when the CME passed three months after the initial eruption, and it may be detectable in the data. Voyager 2 has data that can be interpreted as the passing of the CME, 17 months after. The Curiosity rover's RAD instrument, Mars Odyssey, Rosetta and Cassini showed a sudden decrease in galactic cosmic rays (Forbush decrease) as the CME's protective bubble passed by.[52][53]

Stellar coronal mass ejections

There have been a small number of CMEs observed on other stars, all of which as of 2016[update] have been found on red dwarfs.[54] These have been detected mainly by spectroscopy, most often by studying Balmer lines: the material ejected toward the observer causes asymmetry in the blue wing of the line profiles due to Doppler shift.[55] This enhancement can be seen in absorption when it occurs on the stellar disc (the material is cooler than its surroundings), and in emission when it is outside the disc. The observed projected velocities of CMEs range from ≈84 to 5,800 km/s (52 to 3,600 mi/s).[56][57] There are few stellar CME candidates in shorter wavelengths in UV or X-ray data.[58][59][60][61] Compared to activity on the Sun, CME activity on other stars seems to be far less common.[55][62] The low number of stellar CME detections can be caused by lower intrinsic CME rates compared to the models (e.g. due to magnetic suppression), projection effects, or overestimated Balmer signatures because of the unknown plasma parameters of the stellar CMEs.[63]

See also

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