Context. Coronal mass ejections (CMEs) are major eruptive events on the Sun that result in ejection of large-scale magnetic clouds (MCs) interplanetary space, consisting plasma with enhanced fields whose direction changes coherently when measured situ. The severity CME-induced geomagnetic perturbations and space weather impacts depends strength field (IMF), as well speed duration passage cloud ...

Predictions of coronal mass ejections (CMEs) and solar energetic particles (SEPs) are a central issue in space weather forecasting. In recent years, interest predictions has expanded to include impacts at other planets beyond Earth as well spacecraft scattered throughout the heliosphere. this sense, scope science now encompasses whole heliospheric system, multi-point measurements transients can...

[1] We investigate the relation between Forbush cosmic ray decrease recovery time and coronal mass ejection transit time between the Sun and Earth. We identify 17 Forbush decreases from ground-based neutron count rates between 1978 and 2003 that occur during the same phase in the solar cycle and can be associated with single coronal mass ejections (CMEs) in the SOHO LASCO CME Catalog or previou...

The initiation and evolution of the coronal mass ejection, which occurred on 1998 May 2 in NOAA Active Region 8210, are modeled using a fully three-dimensional, global MHD code. The initial magnetic field for the model is based on magnetogram data from the Wilcox Solar Observatory, and the solar eruption is initiated by slowly evolving the boundary conditions until a critical point is reached w...

Detection and tracking of CMEs is an important issue in solar physics. The appropriate images are continuously collected and parameters describing the extent, position, and time of occurrence of the CMEs are put in a catalogue. Because of the huge amount of data, it is imperative to process these images automatically. One of the best techniques for object extraction is the watershed segmentatio...

Some of the major challenges faced in understanding early evolution Coronal Mass Ejections (CMEs) are due to limited observations inner corona ($<\,3$ R$_{\odot}$) and plane sky measurements. In this work, we have thus extended application Graduated Cylindrical Shell (GCS) model coronal from ground--based coronagraph K--Cor Mauna Loa Solar Observatory (MLSO) along with pair COR--1 onboard Terre...

Two questions about the solar magnetic field might be answered together once their connection is identified. The first is important for large scale dynamo theory: what prevents the magnetic backreaction forces from shutting down the dynamo cycle? The second question is: what determines the handedness of twist and writhe in magnetized coronal ejecta? Magnetic helicity conservation is important f...

We investigate the relation between Forbush cosmic ray decrease recovery time, and coronal mass ejection angular size and transit time between the Sun and Earth. We identify 10 Forbush decreases from ground based neutron count rates between 1997 and 2000, with the addition of the Halloween 2003 event, that can be associated with single coronal mass ejections (CMEs) in the SOHO LASCO CME Catalog...

The twin Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) COR2 coronagraphs of the Solar Terrestrial Relations Observatory (STEREO) provide images of the solar corona from two view points in the solar system. Since their launch in late 2006, the STEREO Ahead (A) and Behind (B) spacecrafts have been slowly separating from Earth at a rate of 22.5 degrees per year. By the end o...

We examine the early phases of two near-limb filament destabilizations involved in coronal mass ejections on 16 June and 27 July 2005, using high-resolution, highcadence observations made with the Transition Region and Coronal Explorer (TRACE), complemented by coronagraphic observations by Mauna Loa and the SOlar and Heliospheric Observatory (SOHO). The filaments’ heights above the solar limb i...