X-Ray Jet Dynamics in a Polar Coronal Hole Region

Filippov, B. P.; Golub, L.; Koutchmy, S.

doi:10.1007/s11207-008-9305-6

Cited by 65 publications

(59 citation statements)

References 41 publications

(29 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…On the other hand, rapid changes in the flux distribution in the corona can be caused by instabilities of pre-existing coronal flux ropes. The presence of flux ropes in jet source regions and their eruption during jet formation is supposed in many blowout jet events (Filippov et al 2009;Moore et al 2010;Liu et al 2011;Shen et al 2011;Schmieder et al 2013) and used as a jet driver in many models (Archontis & Hood 2013;Lee et al 2015). However, observations of the pre-existing flux ropes (as filaments) are few (Shen et al 2012;Filippov et al 2013).…”

Section: Discussionmentioning

confidence: 99%

Formation of a rotating jet during the filament eruption on 2013 April 10–11

Filippov

Srivastava

Dwivedi

et al. 2015

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We analyze multi-wavelength and multi-viewpoint observations of a helically twisted plasma jet formed during a confined filament eruption on 10-11 April 2013. Given a rather large scale event with its high spatial and temporal resolution observations, it allows us to clearly understand some new physical details about the formation and triggering mechanism of twisting jet. We identify a pre-existing flux rope associated with a sinistral filament, which was observed several days before the event. The confined eruption of the filament within a null point topology, also known as an Eiffel tower (or inverted-Y) magnetic field configuration results in the formation of a twisted jet after the magnetic reconnection near a null point. The sign of helicity in the jet is found to be the same as that of the sign of helicity in the filament. Untwisting motion of the reconnected magnetic field lines gives rise to the accelerating plasma along the jet axis. The event clearly shows the twist injection from the pre-eruptive magnetic field to the jet.

show abstract

Section: Discussionmentioning

confidence: 99%

Formation of a rotating jet during the filament eruption on 2013 April 10–11

Filippov

Srivastava

Dwivedi

et al. 2015

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…Article published by EDP Sciences A96, page 1 of 8 A&A 579, A96 (2015) Filippov et al (2009) discuss the formation of jets and proposed scenarios that explain the main features of the events: the relationship with the expected surface magnetism, the rapid and sudden radial motion, and possibly the heating, based on the assumption that the jet occurs above a null point of the coronal magnetic field. Using the Solar Terrestrial Relations Observatory (STEREO; Kaiser et al 2008) twin inner coronagraphs (COR1; Thompson et al 2003) Nisticò et al (2009 studied various aspects of jets, including their correlation with underlying small scale chromospheric bright points.…”

Section: Introductionmentioning

confidence: 99%

Physical properties of solar polar jets

Paraschiv

Бемпорад

Sterling

2015

A&A

View full text Add to dashboard Cite

Aims. The target of this work is to investigate the physical nature of polar jets in the solar corona and their possible contribution to coronal heating and solar wind flow based on the analysis of X-ray images acquired by the Hinode XRT telescope. We estimate the different forms of energy associated with many of these small-scale eruptions, in particular the kinetic energy and enthalpy. Methods. Two Hinode XRT campaign datasets focusing on the two polar coronal holes were selected to analyze the physical properties of coronal jets; the analyzed data were acquired using a series of three XRT filters. Typical kinematical properties (e.g., length, thickness, lifetime, ejection rate, and velocity) of 18 jets are evaluated from the observed sequences, thus providing information on their possible contribution to the fast solar wind flux escaping from coronal holes. Electron temperatures and densities of polar-jet plasmas are also estimated using ratios of the intensities observed in different filters. Results. We find that the largest amount of energy eventually provided to the corona is thermal. The energy due to waves may also be significant, but its value is comparatively uncertain. The kinetic energy is lower than thermal energy, while other forms of energy are comparatively low. Lesser and fainter events seem to be hotter, thus the total contribution by polar jets to the coronal heating could have been underestimated so far. The kinetic energy flux is usually around three times smaller than the enthalpy counterpart, implying that this energy is converted into plasma heating more than in plasma acceleration. This result suggests that the majority of polar jets are most likely not escaping from the Sun and that only cooler ejections could possibly have enough kinetic energy to contribute to the total solar wind flow.

show abstract

“…The lifetimes of CBPs (2−48 h) are proportional to the magnetic flux of the corresponding bipoles in the photosphere (Golub et al 1977) and the EUV intensities (Chandrashekhar et al 2013). At the boundaries of active regions and coronal holes, CBPs are often associated with fast jets when newly emerging flux encounters pre-existing magnetic field lines with opposite polarity and interchange magnetic reconnection occurs, which plays an important role in the dynamic evolution of coronal holes and the slow solar wind (Culhane et al 2007;Filippov et al 2009;Subramanian et al 2010;Madjarska et al 2012;Lee et al 2013;Archontis & Hood 2013;Moore et al 2010Moore et al , 2013Moreno-Insertis & Galsgaard 2013;Zhang & Ji 2014a,b). It has been proposed that magnetic reconnection is responsible for the heating of CBPs Parnell et al 1994;van Driel-Gesztelyi et al 1996;Longcope 1998;Santos et al 2008).…”

Section: Introductionmentioning

confidence: 99%

Reciprocatory magnetic reconnection in a coronal bright point

Zhang

Chen

Ding

et al. 2014

A&A

View full text Add to dashboard Cite

Context. Coronal bright points (CBPs) are small-scale and long-duration brightenings in the lower solar corona. They are often explained in terms of magnetic reconnection. Aims. We aim to study the substructures of a CBP and clarify the relationship among the brightenings of different patches inside the CBP. Methods. The event was observed by the X-ray Telescope (XRT) aboard the Hinode spacecraft on 2009 August 22−23. Results. The CBP showed repeated brightenings (or CBP flashes). During each of the two successive CBP flashes, that is, weak and strong flashes that were separated by ∼2 hr, the XRT images revealed that the CBP was composed of two chambers, patches A and B. During the weak flash, patch A brightened first, and patch B brightened ∼2 min later. During the transition, the right leg of a large-scale coronal loop drifted from the right side of the CBP to the left side. During the strong flash, patch B brightened first, and patch A brightened ∼2 min later. During the transition, the right leg of the large-scale coronal loop drifted from the left side of the CBP to the right side. In each flash, the rapid change of the connectivity of the large-scale coronal loop is strongly suggestive of the interchange reconnection. Conclusions. For the first time we found reciprocatory reconnection in the CBP, which means that reconnected loops in the outflow region of the first reconnection process serve as the inflow of the second reconnection process.

show abstract

X-Ray Jet Dynamics in a Polar Coronal Hole Region

Cited by 65 publications

References 41 publications

Formation of a rotating jet during the filament eruption on 2013 April 10–11

Formation of a rotating jet during the filament eruption on 2013 April 10–11

Physical properties of solar polar jets

Reciprocatory magnetic reconnection in a coronal bright point

Contact Info

Product

Resources

About