A Two-sided Loop X-Ray Solar Coronal Jet Driven by a Minifilament Eruption

Abstract

Most of the commonly discussed solar coronal jets are of the type consisting of a single spire extending approximately vertically from near the solar surface into the corona. Recent research supports that eruption of a miniature filament (minifilament) drives many such single-spire jets, and concurrently generates a miniflare at the eruption site. A different type of coronal jet, identified in Xray images during the Yohkoh era, are two-sided-loop jets, which extend from a central excitation location in opposite directions, along low-lying coronal loops more-or-less horizontal to the surface. We observe such a two-sided-loop jet from the edge of active region (AR) 12473, using data from Hinode XRT and EIS, and SDO AIA and HMI. Similar to single-spire jets, this two-sided-loop jet results from eruption of a minifilament, which accelerates to over 140 km s −1 before abruptly stopping after striking overlying nearly-horizontal loop field at ∼30,000 km altitude and producing the two-sided-loop jet. Analysis of EIS raster scans show that a hot brightening, consistent with a small flare, develops in the aftermath of the eruption, and that Doppler motions (∼40 km s −1 ) occur near the jet-formation region. As with many single-spire jets, the magnetic trigger here is apparently flux cancelation, which occurs at a rate of ∼4×10 18 Mx/hr, comparable to the rate observed in some single-spire AR jets. An apparent increase in the (line-of-sight) flux occurs within minutes of onset of the minifilament eruption, consistent with the apparent increase being due to a rapid reconfiguration of low-lying field during and soon after minifilament-eruption onset.In addition to single-spire jets, there are also two-sided-loop coronal jets (Shibata et al.

Solar Jets: SDO and IRIS Observations in the Perspective of New MHD Simulations

“…The two-sided loop jets exhibit diverging flows from their excitation center. This new kind of jet was also observed with Hinode/XRT and EIS instruments, which confirmed that the opposite direction flows via Dopplershifts (Sterling et al, 2019).…”

Observation and modelling of solar jets

“…So far, the finding of blowout jets has been confirmed by many observational studies, and now we recognize that the vast majority of solar jets are caused by magnetic flux cancellation rather than flux emergence [63,[69][70][71][72][73][74][75][76][77][78][79][80][81][82][83][84]. Recently, high-resolution observational studies have shown that two-sided-loop jets are also associated with flux cancellations and include the eruption of mini-filaments inside the base arches [44,46,49,85,86], and two-sidedloop jets occurring in filament channels may be important for causing the eruption of large filaments [87].…”

“…An anemone jet exhibits an inverted-Y shape consisting of a straight plasma beam and a bright dome-like base. By contrast, a two-sided-loop jet appears as a pair of plasma beams ejecting in opposite directions from the eruption source region [44][45][46][47][48][49]. Recently, high-resolution observations combined with extrapolated three-dimensional (3D) coronal magnetic fields revealed the fan-spine topology magnetic system of straight anemone jets [50], which consists of a coronal nullpoint, a dome-like fan that represents the [51][52][53][54][55][56][57][58][59][60].…”

Coronal microjets in quiet-Sun regions observed with the Extreme Ultraviolet Imager onboard Solar Orbiter

“…Solar jets are one type of pervasive and explosive phenomena on the Sun, usually appearing Corresponding author: Hui Tian huitian@pku.edu.cn as a footpoint brightening followed by a nearly collimated plasma ejection (e.g., Raouafi et al 2016;Shen 2021;Zheng et al 2018). Coronal jets are often observed in extreme ultraviolet (EUV, e.g., Nisticò et al 2009;Yang et al 2011;Srivastava et al 2012;Chandrashekhar et al 2014b;Kumar et al 2018Kumar et al , 2019a and X-ray passbands (e.g., Shimojo et al 1996;Sterling et al 2019) in active regions (ARs) and coronal holes. These coronal jets normally appear as anemone jets (i.e., inverted-Y or λ shape, e.g., Cirtain et al 2007;Nisticò et al 2009) or two-sided-loop jets (e.g., Tian et al 2017;Wei et al 2020).…”