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A Vourlidas - One of the best experts on this subject based on the ideXlab platform.
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multi viewpoint Coronal Mass Ejection catalog based on stereo cor2 observations
The Astrophysical Journal, 2017Co-Authors: A Vourlidas, L Balmaceda, G Stenborg, Alisson Dal LagoAbstract:We present the first multi-viewpoint Coronal Mass Ejection (CME) catalog. The events are identified visually in simultaneous total brightness observations from the twin SECCHI/COR2 coronagraphs on board the Solar Terrestrial Relations Observatory mission. The Multi-View CME Catalog differs from past catalogs in three key aspects: (1) all events between the two viewpoints are cross-linked, (2) each event is assigned a physics-motivated morphological classification (e.g., jet, wave, and flux rope), and (3) kinematic and geometric information is extracted semi-automatically via a supervised image segmentation algorithm. The database extends from the beginning of the COR2 synoptic program (2007 March) to the end of dual-viewpoint observations (2014 September). It contains 4473 unique events with 3358 events identified in both COR2s. Kinematic properties exist currently for 1747 events (26% of COR2-A events and 17% of COR2-B events). We examine several issues, made possible by this cross-linked CME database, including the role of projection on the perceived morphology of events, the missing CME rate, the existence of cool material in CMEs, the solar cycle dependence on CME rate, speeds and width, and the existence of flux rope within CMEs. We discuss the implications for past single-viewpoint studies and for Space Weather research. The database is publicly available on the web including all available measurements. We hope that it will become a useful resource for the community.
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chromosphere to 1 au simulation of the 2011 march 7th event a comprehensive study of Coronal Mass Ejection propagation
arXiv: Solar and Stellar Astrophysics, 2016Co-Authors: Meng Jin, A Vourlidas, W B Manchester, G Toth, I V Sokolov, B Van Der Holst, C A De Koning, T I GombosiAbstract:We perform and analyze results of a global magnetohydrodyanmic (MHD) simulation of the fast Coronal Mass Ejection (CME) that occurred on 2011 March 7. The simulation is made using the newly developed Alfven Wave Solar Model (AWSoM), which describes the background solar wind starting from the upper chromosphere and extends to 24 R$_{\odot}$. Coupling AWSoM to an inner heliosphere (IH) model with the Space Weather Modeling Framework (SWMF) extends the total domain beyond the orbit of Earth. Physical processes included in the model are multi-species thermodynamics, electron heat conduction (both collisional and collisionless formulations), optically thin radiative cooling, and Alfven-wave turbulence that accelerates and heats the solar wind. The Alfven-wave description is physically self-consistent, including non-Wentzel-Kramers-Brillouin (WKB) reflection and physics-based apportioning of turbulent dissipative heating to both electrons and protons. Within this model, we initiate the CME by using the Gibson-Low (GL) analytical flux rope model and follow its evolution for days, in which time it propagates beyond STEREO A. A detailed comparison study is performed using remote as well as \textit{in situ} observations. Although the flux rope structure is not compared directly due to lack of relevant ejecta observation at 1 AU in this event, our results show that the new model can reproduce many of the observed features near the Sun (e.g., CME-driven extreme ultraviolet (EUV) waves, deflection of the flux rope from the Coronal hole, "double-front" in the white light images) and in the heliosphere (e.g., shock propagation direction, shock properties at STEREO A).
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relationship of euv irradiance Coronal dimming slope and depth to Coronal Mass Ejection speed and Mass
The Astrophysical Journal, 2016Co-Authors: James Paul Mason, B J Thompson, R C Colaninno, Thomas N Woods, D F Webb, A VourlidasAbstract:Extreme ultraviolet (EUV) Coronal dimmings are often observed in response to solar eruptive events. These phenomena can be generated via several different physical processes. For space weather, the most important of these is the temporary void left behind by a Coronal Mass Ejection (CME). Massive, fast CMEs tend to leave behind a darker void that also usually corresponds to minimum irradiance for the cooler Coronal emissions. If the dimming is associated with a solar are, as is often the case, the are component of the irradiance light curve in the cooler Coronal emission can be isolated and removed using simultaneous measurements of warmer Coronal lines. We apply this technique to 37dimming events identified during two separate two-week periods in 2011, plus an event on 2010 August 7 analyzed in a previous paper, to parameterize dimming in terms of depth and slope. We provide statistics on which combination of wavelengths worked best for the flare-removal method, describe the fitting methods applied to the dimming light curves, and compare the dimming parameters with corresponding CME parameters of Mass and speed. The best linear relationships found are nu(sub CME) [km/s] approx. equals 2.36 x 10 6 [km/%] x s(sub dim) [%/s] m(sub CME) [g] approx. equals 2.59 x 10(exp.15 [g/%] x the square root of d(sub dim) [%].These relationships could be used for space weather operations of estimating CME Mass and speed using near-real-time irradiance dimming measurements.
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relationship of euv irradiance Coronal dimming slope and depth to Coronal Mass Ejection speed and Mass
arXiv: Solar and Stellar Astrophysics, 2016Co-Authors: James Paul Mason, B J Thompson, R C Colaninno, Thomas N Woods, D F Webb, A VourlidasAbstract:Extreme ultraviolet (EUV) Coronal dimmings are often observed in response to solar eruptive events. These phenomena can be generated via several different physical processes. For space weather, the most important of these is the temporary void left behind by a Coronal Mass Ejection (CME). Massive, fast CMEs tend to leave behind a darker void that also usually corresponds to minimum irradiance for the cooler Coronal emissions. If the dimming is associated with a solar flare, as is often the case, the flare component of the irradiance light curve in the cooler Coronal emission can be isolated and removed using simultaneous measurements of warmer Coronal lines. We apply this technique to 37 dimming events identified during two separate two-week periods in 2011, plus an event on 2010 August 7 analyzed in a previous paper, to parameterize dimming in terms of depth and slope. We provide statistics on which combination of wavelengths worked best for the flare-removal method, describe the fitting methods applied to the dimming light curves, and compare the dimming parameters with corresponding CME parameters of Mass and speed. The best linear relationships found are $$ \begin{align} v_{CME} \Big[\frac{km}{s} \Big] & \approx 2.36 \times 10^6 \Big[\frac{km}{\%} \Big] \times s_{dim} \Big[\frac{\%}{s} \Big] \\ m_{CME} [g] & \approx 2.59 \times 10^{15} \Big[\frac{g}{\%} \Big] \times \sqrt{d_{dim}} [\%]. \end{align} $$ These relationships could be used for space weather operations of estimating CME Mass and speed using near-realtime irradiance dimming measurements.
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remote and in situ observations of an unusual earth directed Coronal Mass Ejection from multiple viewpoints
Journal of Geophysical Research, 2012Co-Authors: T Nieveschinchilla, A Vourlidas, R C Colaninno, A Szabo, R P Lepping, S A Boardsen, B J Anderson, H KorthAbstract:[1] During June 16–21, 2010, an Earth-directed Coronal Mass Ejection (CME) event was observed by instruments onboard STEREO, SOHO, MESSENGER and Wind. This event was the first direct detection of a rotating CME in the middle and outer corona. Here, we carry out a comprehensive analysis of the evolution of the CME in the interplanetary medium comparing in situ and remote observations, with analytical models and three-dimensional reconstructions. In particular, we investigate the parallel and perpendicular cross section expansion of the CME from the corona through the heliosphere up to 1 AU. We use height-time measurements and the Gradual Cylindrical Shell (GCS) technique to model the imaging observations, remove the projection effects, and derive the 3-dimensional extent of the event. Then, we compare the results with in situ analytical Magnetic Cloud (MC) models, and with geometrical predictions from past works. We find that the parallel (along the propagation plane) cross section expansion agrees well with the in situ model and with the Bothmer and Schwenn (1998) empirical relationship based on in situ observations between 0.3 and 1 AU. Our results effectively extend this empirical relationship to about 5 solar radii. The expansion of the perpendicular diameter agrees very well with the in situ results at MESSENGER (∼0.5 AU) but not at 1 AU. We also find a slightly different, from Bothmer and Schwenn (1998), empirical relationship for the perpendicular expansion. More importantly, we find no evidence that the CME undergoes a significant latitudinal over-expansion as it is commonly assumed. Instead, we find evidence that effects due to CME rotation and expansion can be easily confused in the images leading to a severe overestimation of the proper 3D size of the event. Finally, we find that the reconstructions of the CME morphology from the in situ observations at 1 AU are in agreement with the remote sensing observations but they show a big discrepancy at MESSENGER. We attribute this discrepancy to the ambiguity of selecting the proper boundaries due to the lack of accompanying plasma measurements.
Ying Liu - One of the best experts on this subject based on the ideXlab platform.
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kinetic properties of an interplanetary shock propagating inside a Coronal Mass Ejection
The Astrophysical Journal, 2018Co-Authors: Mingzhe Liu, Ying Liu, Zhongwei Yang, L B WilsonAbstract:We investigate the kinetic properties of a typical fast-mode shock inside an interplanetary Coronal Mass Ejection (ICME) observed on 1998 August 6 at 1 au, including particle distributions and wave analysis with the in situ measurements from Wind. Key results are obtained concerning the shock and the shock–ICME interaction at kinetic scales: (1) gyrating ions, which may provide energy dissipation at the shock in addition to wave-particle interactions, are observed around the shock ramp; (2) despite the enhanced proton temperature anisotropy of the shocked plasma, the low plasma β inside the ICME constrains the shocked plasma under the thresholds of the ion cyclotron and mirror-mode instabilities; (3) whistler heat flux instabilities, which can pitch-angle scatter halo electrons through a cyclotron resonance, are observed around the shock, and can explain the disappearance of bi-directional electrons (BDEs) inside the ICME together with normal betatron acceleration; (4) whistler waves near the shock are likely associated with the whistler heat flux instabilities excited at the shock ramp, which is consistent with the result that the waves may originate from the shock ramp; (5) the whistlers share a similar characteristic with the shocklet whistlers observed by Wilson et al., providing possible evidence that the shock is decaying because of the strong magnetic field inside the ICME.
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sun to earth characteristics of the 2012 july 12 Coronal Mass Ejection and associated geo effectiveness
arXiv: Solar and Stellar Astrophysics, 2016Co-Authors: Ying Liu, Rui Wang, Christian Mostl, Zhongwei YangAbstract:We analyze multi-spacecraft observations associated with the 2012 July 12 Coronal Mass Ejection (CME), covering the source region on the Sun from SDO, stereoscopic imaging observations from STEREO, magnetic field characteristics at MESSENGER, and type II radio burst and in situ measurements from Wind. A triangulation method based on STEREO stereoscopic observations is employed to determine the kinematics of the CME, and the outcome is compared with the result derived from the type II radio burst with a solar wind electron density model. A Grad-Shafranov technique is applied to Wind in situ data to reconstruct the flux-rope structure and compare it with the observation of the solar source region, which helps understand the geo-effectiveness associated with the CME structure. Conclusions are as follows: (1) the CME undergoes an impulsive acceleration, a rapid deceleration before reaching MESSENGER, and then a gradual deceleration out to 1 AU, which should be noticed in CME kinematics models; (2) the type II radio burst was probably produced from a high-density interaction region between the CME-driven shock and a nearby streamer or from the shock flank with lower heights, which implies uncertainties in the determination of CME kinematics using solely type II radio bursts; (3) the flux-rope orientation and chirality deduced from in situ reconstruction at Wind agree with those obtained from solar source observations; (4) the prolonged southward magnetic field near the Earth is mainly from the axial component of the largely southward inclined flux rope, which indicates the importance of predicting both the flux-rope orientation and magnetic field components in geomagnetic activity forecasting.
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THE ROLE OF ACTIVE REGION Coronal MAGNETIC FIELD IN DETERMINING Coronal Mass Ejection PROPAGATION DIRECTION
The Astrophysical Journal, 2015Co-Authors: Rui Wang, Ying Liu, Xinghua Dai, Zhongwei Yang, Chong HuangAbstract:We study the role of the Coronal magnetic field configuration of an active region (AR) in determining the propagation direction of a Coronal Mass Ejection (CME). The CME occurred in the AR 11944 (S09W01) near the disk center on 2014 January 7 and was associated with an X1.2 flare. A new CME reconstruction procedure based on a polarimetric technique is adopted, which shows that the CME changed its propagation direction by around 28° in latitude within 2.5 and 43° in longitude within 6.5 with respect to the CME source region. This significant non-radial motion is consistent with the finding of Mostl et al. We use nonlinear force-free field and potential field source surface extrapolation methods to determine the configurations of the Coronal magnetic field. We also calculate the magnetic energy density distributions at different heights based on the extrapolations. Our results show that the AR Coronal magnetic field has a strong influence on the CME propagation direction. This is consistent with the "channeling" by the AR Coronal magnetic field itself, rather than deflection by nearby structures. These results indicate that the AR Coronal magnetic field configuration has to be taken into account in order to determine CME propagation direction correctly.
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The role of active region Coronal magnetic field in determining Coronal Mass Ejection propagation direction
arXiv: Solar and Stellar Astrophysics, 2015Co-Authors: Rui Wang, Ying Liu, Xinghua Dai, Zhongwei Yang, Chong HuangAbstract:We study the role of the Coronal magnetic field configuration of an active region in determining the propagation direction of a Coronal Mass Ejection (CME). The CME occurred in the active region 11944 (S09W01) near the disk center on 2014 January 7 and was associated with an X1.2 flare. A new CME reconstruction procedure based on a polarimetric technique is adopted, which shows that the CME changed its propagation direction by around 28$^\circ$ in latitude within 2.5 R$_\odot$ and 43$^\circ$ in longitude within 6.5 R$_\odot$ with respect to the CME source region. This significant non-radial motion is consistent with the finding of M$\ddot{o}$stl et al. (2015). We use nonlinear force-free field (NLFFF) and potential field source surface (PFSS) extrapolation methods to determine the configurations of the Coronal magnetic field. We also calculate the magnetic energy density distributions at different heights based on the extrapolations. Our results show that the active region Coronal magnetic field has a strong influence on the CME propagation direction. This is consistent with the "channelling" by the active region Coronal magnetic field itself, rather than deflection by nearby structures. These results indicate that the active region Coronal magnetic field configuration has to be taken into account in order to determine CME propagation direction correctly.
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radio signatures of Coronal Mass Ejection streamer interaction and source diagnostics of type ii radio burst
The Astrophysical Journal, 2012Co-Authors: Hongqiang Song, Shiwei Feng, Yao Chen, Xiangliang Kong, Xueshang Feng, Ying LiuAbstract:It has been suggested that type II radio bursts are due to energetic electrons accelerated at Coronal shocks. Radio observations, however, have poor or no spatial resolutions to pinpoint the exact acceleration locations of these electrons. In this paper, we discuss a promising approach to infer the electron acceleration location by combining radio and white light observations. The key assumption is to relate specific morphological features (e.g., spectral bumps) of the dynamic spectra of type II radio bursts to imaging features (e.g., Coronal Mass Ejection (CME) going into a streamer) along the CME (and its driven shock) propagation. In this study, we examine the CME-streamer interaction for the solar eruption dated on 2003 November 1. The presence of spectral bump in the relevant type II radio burst is identified, which is interpreted as a natural result of the shock-radio-emitting region entering the dense streamer structure. The study is useful for further determinations of the location of type II radio burst and the associated electron acceleration by CME-driven shock.
G Stenborg - One of the best experts on this subject based on the ideXlab platform.
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multi viewpoint Coronal Mass Ejection catalog based on stereo cor2 observations
The Astrophysical Journal, 2017Co-Authors: A Vourlidas, L Balmaceda, G Stenborg, Alisson Dal LagoAbstract:We present the first multi-viewpoint Coronal Mass Ejection (CME) catalog. The events are identified visually in simultaneous total brightness observations from the twin SECCHI/COR2 coronagraphs on board the Solar Terrestrial Relations Observatory mission. The Multi-View CME Catalog differs from past catalogs in three key aspects: (1) all events between the two viewpoints are cross-linked, (2) each event is assigned a physics-motivated morphological classification (e.g., jet, wave, and flux rope), and (3) kinematic and geometric information is extracted semi-automatically via a supervised image segmentation algorithm. The database extends from the beginning of the COR2 synoptic program (2007 March) to the end of dual-viewpoint observations (2014 September). It contains 4473 unique events with 3358 events identified in both COR2s. Kinematic properties exist currently for 1747 events (26% of COR2-A events and 17% of COR2-B events). We examine several issues, made possible by this cross-linked CME database, including the role of projection on the perceived morphology of events, the missing CME rate, the existence of cool material in CMEs, the solar cycle dependence on CME rate, speeds and width, and the existence of flux rope within CMEs. We discuss the implications for past single-viewpoint studies and for Space Weather research. The database is publicly available on the web including all available measurements. We hope that it will become a useful resource for the community.
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the first observation of a rapidly rotating Coronal Mass Ejection in the middle corona
The Astrophysical Journal, 2011Co-Authors: A Vourlidas, R C Colaninno, T Nieveschinchilla, G StenborgAbstract:In this Letter, we present the first direct detection of a rotating Coronal Mass Ejection (CME) in the middle corona (5-15 R ?). The CME rotation rate is 60? day-1, which is the highest rate reported yet. The Earth-directed event was observed by the STEREO/SECCHI and SOHO/LASCO instruments. We are able to derive the three-dimensional morphology and orientation of the CME flux rope by applying a forward-fitting model to simultaneous observations from three vantage points (SECCHI-A, -B, LASCO). Surprisingly, we find that even such rapidly rotating CME does not result in significant projection effects (variable angular width) in any single coronagraph view. This finding may explain the prevalent view of constant angular width for CMEs above 5 R ? and the lack of detections of rotating CMEs in the past. Finally, the CME is a stealth CME with very weak low corona signatures as viewed from Earth. It originated from a quiet-Sun neutral line. We tentatively attribute the fast rotation to a possible disconnection of one of the CME footpoints early in the eruption. We discuss the implications of such rotations to space weather prediction.
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the genesis of an impulsive Coronal Mass Ejection observed at ultra high cadence by aia on sdo
The Astrophysical Journal, 2010Co-Authors: S Patsourakos, A Vourlidas, G StenborgAbstract:The study of fast, eruptive events in the low solar corona is one of the science objectives of the Atmospheric Imaging Assembly (AIA) imagers on the recently launched Solar Dynamics Observatory (SDO), which take full disk images in 10 wavelengths with arcsecond resolution and 12 s cadence. We study with AIA the formation of an impulsive Coronal Mass Ejection (CME) which occurred on 2010 June 13 and was associated with an M1.0 class flare. Specifically, we analyze the formation of the CME EUV bubble and its initial dynamics and thermal evolution in the low corona using AIA images in three wavelengths (171 A, 193 A, and 211 A). We derive the first ultra-high cadence measurements of the temporal evolution of the CME bubble aspect ratio (=bubble height/bubble radius). Our main result is that the CME formation undergoes three phases: it starts with a slow self-similar expansion followed by a fast but short-lived (~70 s) period of strong lateral overexpansion which essentially creates the CME. Then the CME undergoes another phase of self-similar expansion until it exits the AIA field of view. During the studied interval, the CME height-time profile shows a strong, short-lived, acceleration followed by deceleration. The lateral overexpansion phase coincides with the deceleration phase. The impulsive flare heating and CME acceleration are closely coupled. However, the lateral overexpansion of the CME occurs during the declining phase and is therefore not linked to flare reconnection. In addition, the multi-thermal analysis of the bubble does not show significant evidence of temperature change.
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the genesis of an impulsive Coronal Mass Ejection observed at ultra high cadence by aia on sdo
arXiv: Solar and Stellar Astrophysics, 2010Co-Authors: S Patsourakos, A Vourlidas, G StenborgAbstract:The study of fast, eruptive events in the low solar corona is one of the science objectives of the Atmospheric Imaging Assembly (AIA) imagers on the recently launched Solar Dynamics Observatory (SDO), which take full disk images in ten wavelengths with arcsecond resolution and 12 sec cadence. We study with AIA the formation of an impulsive Coronal Mass Ejection (CME) which occurred on June 13, 2010 and was associated with an M1.0 class flare. Specifically, we analyze the formation of the CME EUV bubble and its initial dynamics and thermal evolution in the low corona using AIA images in three wavelengths (171, 193 and 211 A). We derive the first ultra-high cadence measurements of the temporal evolution of the CME bubble aspect ratio (=bubble-height/bubble-radius). Our main result is that the CME formation undergoes three phases: it starts with a slow self-similar expansion followed by a fast but short-lived (~ 70 sec) period of strong lateral over-expansion which essentially creates the CME. Then the CME undergoes another phase of self-similar expansion until it exits the AIA field of view. During the studied interval, the CME height-time profile shows a strong, short-lived, acceleration followed by deceleration. The lateral overexpansion phase coincides with the deceleration phase. The impulsive flare heating and CME acceleration are closely coupled. However, the lateral overexpansion of the CME occurs during the declining phase and is therefore not linked to flare reconnection. In addition, the multi-thermal analysis of the bubble does not show significant evidence of temperature change.
Shiwei Feng - One of the best experts on this subject based on the ideXlab platform.
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a solar type ii radio burst from Coronal Mass Ejection Coronal ray interaction simultaneous radio and extreme ultraviolet imaging
The Astrophysical Journal, 2014Co-Authors: Yao Chen, Li Feng, Shiwei Feng, Xiangliang Kong, Fan Guo, Bing WangAbstract:Simultaneous radio and extreme ultraviolet (EUV)/white-light imaging data are examined for a solar type II radio burst occurring on 2010 March 18 to deduce its source location. Using a bow-shock model, we reconstruct the three-dimensional EUV wave front (presumably the type-II-emitting shock) based on the imaging data of the two Solar TErrestrial RElations Observatory spacecraft. It is then combined with the Nancay radio imaging data to infer the three-dimensional position of the type II source. It is found that the type II source coincides with the interface between the Coronal Mass Ejection (CME) EUV wave front and a nearby Coronal ray structure, providing evidence that the type II emission is physically related to the CME-ray interaction. This result, consistent with those of previous studies, is based on simultaneous radio and EUV imaging data for the first time.
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radio signatures of Coronal Mass Ejection streamer interaction and source diagnostics of type ii radio burst
The Astrophysical Journal, 2012Co-Authors: Hongqiang Song, Shiwei Feng, Yao Chen, Xiangliang Kong, Xueshang Feng, Ying LiuAbstract:It has been suggested that type II radio bursts are due to energetic electrons accelerated at Coronal shocks. Radio observations, however, have poor or no spatial resolutions to pinpoint the exact acceleration locations of these electrons. In this paper, we discuss a promising approach to infer the electron acceleration location by combining radio and white light observations. The key assumption is to relate specific morphological features (e.g., spectral bumps) of the dynamic spectra of type II radio bursts to imaging features (e.g., Coronal Mass Ejection (CME) going into a streamer) along the CME (and its driven shock) propagation. In this study, we examine the CME-streamer interaction for the solar eruption dated on 2003 November 1. The presence of spectral bump in the relevant type II radio burst is identified, which is interpreted as a natural result of the shock-radio-emitting region entering the dense streamer structure. The study is useful for further determinations of the location of type II radio burst and the associated electron acceleration by CME-driven shock.
D J Mccomas - One of the best experts on this subject based on the ideXlab platform.
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solar energetic particles produced by a slow Coronal Mass Ejection at 0 25 au
Astrophysical Journal Supplement Series, 2020Co-Authors: J Giacalone, A P Rouillard, D G Mitchell, R C Allen, M E Hill, R L Mcnutt, J R Szalay, M I Desai, A Kouloumvakos, D J MccomasAbstract:We present an analysis of Parker Solar Probe (PSP) IS⊙IS observations of ~30–300 keV n⁻¹ ions on 2018 November 11 when PSP was about 0.25 au from the Sun. Five hours before the onset of a solar energetic particle (SEP) event, a Coronal Mass Ejection (CME) was observed by STEREO-A/COR2, which crossed PSP about a day later. No shock was observed locally at PSP, but the CME may have driven a weak shock earlier. The SEP event was dispersive, with higher energy ions arriving before the lower energy ones. Timing suggests the particles originated at the CME when it was at ~7.4R_⊙. SEP intensities increased gradually from their onset over a few hours, reaching a peak, and then decreased gradually before the CME arrived at PSP. The event was weak, having a very soft energy spectrum (−4 to −5 spectral index). The earliest arriving particles were anisotropic, moving outward from the Sun, but later, the distribution was observed to be more isotropic. We present numerical solutions of the Parker transport equation for the transport of 30–300 keV n⁻¹ ions assuming a source comoving with the CME. Our model agrees well with the observations. The SEP event is consistent with ion acceleration at a weak shock driven briefly by the CME close to the Sun, which later dissipated before arriving at PSP, followed by the transport of ions in the interplanetary magnetic field.
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tracking Coronal features from the low corona to earth a quantitative analysis of the 2008 december 12 Coronal Mass Ejection
The Astrophysical Journal, 2013Co-Authors: C E Deforest, D J Mccomas, T A HowardAbstract:We have tracked a slow magnetic cloud associated Coronal Mass Ejection (CME) continuously from its origin as a flux rope structure in the low solar corona over a four-day passage to impact with spacecraft located near Earth. Combining measurements from the STEREO, ACE, and Wind space missions, we are able to follow major elements with enough specificity to relate pre-CME Coronal structure in the low corona to the corresponding elements seen in the near-Earth in situ data. Combining extreme ultraviolet imaging, quantitative Thomson scattering data throughout the flight of the CME, and ground-truth in situ measurements, we: (1) identify the plasma observed by ACE and Wind with specific features in the solar corona (a segment of a long flux rope); (2) determine the onset mechanism of the CME (destabilization of a filament channel following flare reconnection, coupled with the Mass draining instability) and demonstrate that it is consistent with the in situ measurements; (3) identify the origin of different layers of the sheath material around the central magnetic cloud (closed field lifted from the base of the corona, closed field entrained during passage through the corona, and solar wind entrained by the front of the CME); (4) measure Mass accretion of the system via snowplow effects in the solar wind as the CME crossed the solar system; and (5) quantify the kinetic energy budget of the system in interplanetary space, and determine that it is consistent with no long-term driving force on the CME.