The Deceleration of an Interplanetary Transient from the Sun to 5 Au

Tappin, S. J.

doi:10.1007/s11207-006-2065-2

Cited by 80 publications

(98 citation statements)

References 22 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Th is early phase is generally attributed to the Lorentz force whereby the dominant outward magnetic pressure overcomes the internal and / or external magnetic fi eld tension. Th e subsequent increase in velocity, at heights above ~ 7 R for this event, is predicted by theory to result from the eff ects of drag 17 , as the CME is infl uenced by solar wind fl ows of ~ 550 km s − 1 emanating from latitudes տ ± 5 ° of the ecliptic (again from inspection of the Wang-Sheeley-Arge model). At large distances from the Sun, during this postulated drag-dominated epoch of CME propagation, the equation of motion can be cast in the following form:…”

Section: Cme Observation On 12 December 2008mentioning

confidence: 74%

“…Studies that compare in situ CME velocity measurements with initial eruption speeds through the corona show that slow CMEs are accelerated towards the speed of the solar wind, and fast CMEs decelerated 15,16 . It has been suggested that this is due to the eff ects of drag on the CME in the solar wind 17,18 . However, the quanti fi cation of drag, along with that of both CME expansion and non-radial motion, is currently lacking, primarily because of the limits of observations from single fi xed viewpoints with restricted fi elds of view.…”

mentioning

confidence: 99%

See 1 more Smart Citation

Propagation of an Earth-directed coronal mass ejection in three dimensions

et al. 2010

View full text Add to dashboard Cite

Solar coronal mass ejections (CMEs) are the most signifi cant drivers of adverse space weather on Earth, but the physics governing their propagation through the heliosphere is not well understood. Although stereoscopic imaging of CMEs with NASA's Solar Terrestrial Relations Observatory (STEREO) has provided some insight into their three-dimensional (3D) propagation, the mechanisms governing their evolution remain unclear because of diffi culties in reconstructing their true 3D structure. In this paper, we use a new elliptical tie-pointing technique to reconstruct a full CME front in 3D, enabling us to quantify its defl ected trajectory from high latitudes along the ecliptic, and measure its increasing angular width and propagation from 2 to 46 R ( ~ 0.2 AU). Beyond 7 R , we show that its motion is determined by an aerodynamic drag in the solar wind and, using our reconstruction as input for a 3D magnetohydrodynamic simulation, we determine an accurate arrival time at the Lagrangian L1 point near Earth.

show abstract

Section: Cme Observation On 12 December 2008mentioning

confidence: 74%

mentioning

confidence: 99%

Propagation of an Earth-directed coronal mass ejection in three dimensions

et al. 2010

View full text Add to dashboard Cite

show abstract

“…The cause of the increasing mass of the CME is generally accepted as solar wind material that is acreted ahead of the CME driver (its flux rope) as it expands through the heliosphere (e.g., Lugaz et al 2005;Tappin 2006;Howard et al 2007;DeForest et al 2013), as the CME measurements, including those made in the present study, typically include the so-called "sheath" component. This is evidenced by the substantial increase in the density of just the flank of the CME shown in Figure 2.…”

Section: Discussionmentioning

confidence: 95%

Measuring an Eruptive Prominence at Large Distances From the Sun. Ii. Approaching 1 Au

Howard

2015

ApJ

View full text Add to dashboard Cite

The physical properties of eruptive prominences are unknown at large distances from the Sun. They are rarely, if ever, measured by in situ spacecraft and until recently our ability to measure them beyond the fields of view of solar imagers has been severely limited. The data quality of heliospheric imaging has reached a point where some quantitative measurements of prominences are now possible. I present the first such measurements of a bright prominence continually out to distances of around 1 AU from the Sun. This work follows on from the preparatory work presented in an accompanying paper, which showed that that the brightness of a prominence can be safely assumed to arise entirely from Thomson scattering in the STEREO/HI fields of view. Measurements of distance, speed, and mass are provided along with those from its accompanying coronal mass ejection (CME) to demonstrate their geometric, kinematic, and mass relationships. I find that the prominence travels with a slower speed than that of the CME, but its location relative to the CME structure does not conform to the expected location for basic geometric expansion. Further, the mass of the prominence was found to decrease by around an order of magnitude while that of the CME increased by an order of magnitude across the same distance.

show abstract

“…Gopalswamy et al 2000Gopalswamy et al , 2001Vršnak & Gopalswamy 2002;Yashiro et al 2004;Tappin 2006;Manoharan 2006;Vršnak & Žic 2007;Vršnak et al 2008). Taking into account the physical properties of the drag (e.g.…”

Section: Introductionmentioning

confidence: 99%

The role of aerodynamic drag in propagation of interplanetary coronal mass ejections

Vršnak

Žic

Falkenberg

et al. 2010

A&A

122

115

View full text Add to dashboard Cite

Context. The propagation of interplanetary coronal mass ejections (ICMEs) and the forecast of their arrival on Earth is one of the central issues of space weather studies. Aims. We investigate to which degree various ICME parameters (mass, size, take-off speed) and the ambient solar-wind parameters (density and velocity) affect the ICME Sun-Earth transit time. Methods. We study solutions of a drag-based equation of motion by systematically varying the input parameters. The analysis is focused on ICME transit times and 1 AU velocities. Results. The model results reveal that wide ICMEs of low masses adjust to the solar-wind speed already close to the sun, so the transit time is determined primarily by the solar-wind speed. The shortest transit times and accordingly the highest 1 AU velocities are related to narrow and massive ICMEs (i.e. high-density eruptions) propagating in high-speed solar wind streams. We apply the model to the Sun-Earth event associated with the CME of 25 July 2004 and compare the results with the outcome of the numerical MHD modeling.

show abstract

The Deceleration of an Interplanetary Transient from the Sun to 5 Au

Cited by 80 publications

References 22 publications

Propagation of an Earth-directed coronal mass ejection in three dimensions

Propagation of an Earth-directed coronal mass ejection in three dimensions

Measuring an Eruptive Prominence at Large Distances From the Sun. Ii. Approaching 1 Au

The role of aerodynamic drag in propagation of interplanetary coronal mass ejections

Contact Info

Product

Resources

About