We present the analysis of an unusual failed eruption captured in high cadence and in many wavelengths during the observing campaign in support of the VAULT2.0 sounding rocket launch. The refurbished Very high Angular resolution Ultraviolet Telescope (VAULT2.0 ) is a Lyα (λ 1216Å) spectroheliograph launched on September 30, 2014. The campaign targeted active region NOAA AR 12172 and was closely coordinated with the Hinode and IRIS missions and several ground-based observatories (NSO/IBIS, SOLIS, and BBSO). A filament eruption accompanied by a low level flaring event (at the GOES C-class level) occurred around the VAULT2.0 launch. No Coronal Mass Ejection (CME) was observed. The eruption and its source region, however, were recorded by the campaign instruments in many atmospheric heights ranging from the photosphere to the corona in high cadence and spatial resolution. This is a rare occasion which enables -2 -us to perform a comprehensive investigation on a failed eruption. We find that a rising Magnetic Flux Rope-like (MFR) structure was destroyed during its interaction with the ambient magnetic field creating downflows of cool plasma and diffuse hot coronal structures reminiscent of "cusps". We employ magnetofrictional simulations to show that the magnetic topology of the ambient field is responsible for the destruction of the MFR. Our unique observations suggest that the magnetic topology of the corona is a key ingredient for a successful eruption.

We present results from an observing campaign in support of the VAULT2.0 sounding rocket launch on September 30, 2014. VAULT2.0 is a Lyα (1216Å) spectroheliograph capable of providing spectroheliograms at high cadence. Lyα observations are highly complementary to the IRIS observations of the upper chromosphere and the low transition region (TR) but have previously been unavailable. The VAULT2.0 data provide new constraints on upper-chromospheric conditions for numerical models. The observing campaign was closely coordinated with the IRIS mission. Taking advantage of this A new class of spicules (type-II spicules) has been discovered in Hinode/SOT Ca II H observations (De Pontieu et al. 2007). They seem to exhibit much faster speeds as compared to the "traditional" class of type-I spicules (50 − 100 km s −1 ). In Ca II H filtergrams, type-II spicules appear to be shorter lived (typical lifetimes 10-150 s) than type-I spicules whereas for higher chromospheric temperatures, e.g., Mg II h & k formation temperatures or TR temperatures, e.g., Si IV, the lifetimes are 3-10 minutes (Pereira et al. 2014). These spicules are rooted in the chromospheric network and consequently, due to their ubiquity, they are regarded as a significant source of coronal mass and heat transfer (De Pontieu et al. 2009). Tian et al. (2014) studied counterparts to spicules in the IRIS FUV SJI channels and called them "network jets". They measured the plane-of-the-sky speeds with the aid of space-time plots and reported speeds of ≈ 80 to 250 km s −1 . They concluded that due to these very fast speeds, network jets could be a significant source of mass to the solar wind. On the other hand, Rouppe van der Voort et al. (2015) using SST and IRIS observations, studied the heating signatures of on-disk type-II spicules and they found that many type-II spicules

We present meter-wave solar radio spectra of the highest spectro-temporal resolution achieved to date. The observations, obtained with the first station of the Long Wavelength Array (LWA1), show unprecedented detail of solar emissions across a wide bandwidth during a Type-III/IIIb storm. Our flux calibration demonstrates that the LWA1 can detect Type-III bursts much weaker than 1 SFU, much lower than previous observations, and that the distribution of fluxes in these bursts varies with frequency. The high sensitivity and low noise in the data provide strong constraints to models of this type of plasma emission, providing evidence against the idea that Type-IIIb striae are generated from electrons trapped in Langmuir wave sidebands. The continuous generation of electron beams in the corona revealed by the high density Type-III storm is evidence for ubiquitous magnetic reconnection in the lower corona. Such an abundance of reconnection events not only contributes to the total coronal energy budget, but also provides an engine by which to form the populations of seed particles responsible for proton-rich solar energetic particle events. An active region (AR) with such levels of reconnection and the accompanying Type-III/IIIb storms is here proposed to be associated with an increase of SEP production if a CME erupts. The data's constraints on existing theories of Type-IIIb production are used to make an association of the observed Type-IIIb storm to specific electron beam paths with increased inhomogeneities in density, temperature, and/or turbulence. This scenario ties in the observed timing of Type-III and IIIb storms, constrained theories of Type-III and IIIb emission, and the ability of the emitting AR to produce a strong SEP event. The result requires but a single observable to cement these ideas, the statistical correlation of Type-III/IIIb activity with SEP-productive AR.

Very high angular resolution ultraviolet telescope (VAULT2.0) is a Lyman-alpha (Ly[Formula: see text]; 1216[Formula: see text]Å) spectroheliograph designed to observe the upper chromospheric region of the solar atmosphere with high spatial ([Formula: see text]) and temporal (8[Formula: see text]s) resolution. Besides being the brightest line in the solar spectrum, Ly[Formula: see text] emission arises at the temperature interface between coronal and chromospheric plasmas and may, hence, hold important clues about the transfer of mass and energy to the solar corona. VAULT2.0 is an upgrade of the previously flown VAULT rocket and was launched successfully on September 30, 2014 from White Sands Missile Range (WSMR). The target was AR12172 midway toward the southwestern limb. We obtained 33 images at 8[Formula: see text]s cadence at arc second resolution due to hardware problems. The science campaign was a resounding success, with all space and ground-based instruments obtaining high-resolution data at the same location within the AR. We discuss the science rationale, instrument upgrades, and performance during the first flight and present some preliminary science results.

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