Mass Loss in Pre-Main-Sequence Stars via Coronal Mass Ejections and Implications for Angular Momentum Loss

Aarnio, Alicia; Matt, Sean P.; Stassun, Keivan G.

doi:10.1088/0004-637x/760/1/9

Cited by 111 publications

(147 citation statements)

References 75 publications

(103 reference statements)

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“…This work built on earlier theoretical models of time-steady solar wind scaling relations (Cranmer & Saar 2011) and on empirical correlations between CME properties and highenergy flare emissions (e.g., Aarnio et al 2012;Drake et al 2013;Osten & Wolk 2015). Although it is likely that the magnetic properties of a star are more fundamental (i.e., they are what drive the flare and CME properties), it is also undeniable that they are much more difficult to observe than, say, flare light curves.…”

Section: Discussionmentioning

confidence: 99%

“…The large rectangle indicates ages and mass-loss uncertainty limits for the T Tauri stars measured by the Chandra Orion Ultradeep Project (COUP). The ages were estimated by Preibisch & Feigelson (2005) and the CME mass-loss rates were estimated by Aarnio et al (2012). Also shown is a smaller range of uncertainties for EK Dra, a young solar analog whose flaring has been observed extensively.…”

Section: Predicted Mass Loss Historymentioning

confidence: 99%

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Mass-loss Rates from Coronal Mass Ejections: A Predictive Theoretical Model for Solar-type Stars

Cranmer

2017

ApJ

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Coronal mass ejections (CMEs) are eruptive events that cause a solar-type star to shed mass and magnetic flux. CMEs tend to occur together with flares, radio storms, and bursts of energetic particles. On the Sun, CME-related mass loss is roughly an order of magnitude less intense than that of the background solar wind. However, on other types of stars, CMEs have been proposed to carry away much more mass and energy than the time-steady wind. Earlier papers have used observed correlations between solar CMEs and flare energies, in combination with stellar flare observations, to estimate stellar CME rates. This paper sidesteps flares and attempts to calibrate a more fundamental correlation between surface-averaged magnetic fluxes and CME properties. For the Sun, there exists a power-law relationship between the magnetic filling factor and the CME kinetic energy flux, and it is generalized for use on other stars. An example prediction of the time evolution of wind/CME mass-loss rates for a solar-mass star is given. A key result is that for ages younger than about 1 Gyr (i.e., activity levels only slightly higher than the present-day Sun), the CME mass loss exceeds that of the time-steady wind. At younger ages, CMEs carry 10-100 times more mass than the wind, and such high rates may be powerful enough to dispel circumstellar disks and affect the habitability of nearby planets. The cumulative CME mass lost by the young Sun may have been as much as 1% of a solar mass.

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Section: Discussionmentioning

confidence: 99%

Section: Predicted Mass Loss Historymentioning

confidence: 99%

Mass-loss Rates from Coronal Mass Ejections: A Predictive Theoretical Model for Solar-type Stars

Cranmer

2017

ApJ

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“…These are comparable numbers to the typical masses and speeds of solar CMEs (see e.g., the LASCO CME catalogue 9 ). However, much more massive and faster stellar CMEs have been speculated based on the solar flare/CME scaling laws (e.g., Aarnio et al 2012;Drake et al 2013), e.g., masses reaching up 10 19 kg. The stellar CME observed by Houdebine et al (1990), also using the optical spectra, had speed of about 5800 km s −1 .…”

Section: Icmes Beyond the Solar Systemmentioning

confidence: 99%

Coronal mass ejections and their sheath regions in interplanetary space

Kilpua

Koskinen

Pulkkinen

2017

Living Rev Sol Phys

336

360

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Interplanetary coronal mass ejections (ICMEs) are large-scale heliospheric transients that originate from the Sun. When an ICME is sufficiently faster than the preceding solar wind, a shock wave develops ahead of the ICME. The turbulent region between the shock and the ICME is called the sheath region. ICMEs and their sheaths and shocks are all interesting structures from the fundamental plasma physics viewpoint. They are also key drivers of space weather disturbances in the heliosphere and planetary environments. ICME-driven shock waves can accelerate charged particles to high energies. Sheaths and ICMEs drive practically all intense geospace storms at the Earth, and they can also affect dramatically the planetary radiation environments and atmospheres. This review focuses on the current understanding of observational signatures and properties of ICMEs and the associated sheath regions based on five decades of studies. In addition, we discuss modelling of ICMEs and many fundamental outstanding questions on their origin, evolution and effects, largely due to the limitations of single spacecraft observations of these macro-scale structures. We also present current understanding of space weather consequences of these large-scale solar wind structures, including effects at the other Solar System planets and exoplanets. We specially emphasize the different origin, properties and consequences of the sheaths and ICMEs.

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“…In Equation (21), we assumed the maximum CME mass associated with the X10 flare to be~3 10 16 g (Aarnio et al 2012 ( ) . Based on the discussion above, the E y,upperlimit associated with the X10 flare, for example, will be ∼2×10 3 mVm −1 .…”

Section: Super-intense Geomagnetic Storms Associated With Solar Supermentioning

confidence: 99%

“…Coronal mass ejections (CMEs) are the largest plasma explosions in the solar system, and are characterized by a vast amount (typically, 10 10 13 16 -g) of the solar coronal plasma being ejected out into the interplanetary space at speeds up to 3000 kms −1 (Illing & Hundhausen 1986;Aarnio et al 2012;Porfir'eva et al 2012;Webb & Howard 2012).…”

Section: Introductionmentioning

confidence: 99%

Sheath-accumulating Propagation of Interplanetary Coronal Mass Ejection

Takahashi

Shibata

2017

ApJL

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Fast interplanetary coronal mass ejections (ICMEs) are the drivers of strong space weather storms such as solar energetic particle events and geomagnetic storms. The connection between the space-weather-impacting solar wind disturbances associated with fast ICMEs at Earth and the characteristics of causative energetic CMEs observed near the Sun is a key question in the study of space weather storms, as well as in the development of practical space weather prediction. Such shock-driving fast ICMEs usually expand at supersonic speeds during the propagation, resulting in the continuous accumulation of shocked sheath plasma ahead. In this paper, we propose a "sheath-accumulating propagation" (SAP) model that describes the coevolution of the interplanetary sheath and decelerating ICME ejecta by taking into account the process of upstream solar wind plasma accumulation within the sheath region. Based on the SAP model, we discuss (1) ICME deceleration characteristics; (2) the fundamental condition for fast ICMEs at Earth; (3) the thickness of interplanetary sheaths; (4) arrival time prediction; and (5) the super-intense geomagnetic storms associated with huge solar flares. We quantitatively show that not only the speed but also the mass of the CME are crucial for discussing the above five points. The similarities and differences between the SAP model, the drag-based model, and the"snow-plow" model proposed by Tappin are also discussed.

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Mass Loss in Pre-Main-Sequence Stars via Coronal Mass Ejections and Implications for Angular Momentum Loss

Cited by 111 publications

References 75 publications

Mass-loss Rates from Coronal Mass Ejections: A Predictive Theoretical Model for Solar-type Stars

Mass-loss Rates from Coronal Mass Ejections: A Predictive Theoretical Model for Solar-type Stars

Coronal mass ejections and their sheath regions in interplanetary space

Sheath-accumulating Propagation of Interplanetary Coronal Mass Ejection

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