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Following HAWC observations of the Cygnus Cocoon, massive star-forming regions can now be considered to be sources of very-high-energy (TeV to PeV) Galactic cosmic rays.
Using a new infrared spectropolarimeter at Palomar Observatory, the geometry of a number of supernova ejecta have been assessed, revealing a potential similarity in geometry between SN 2018hna and SN 1987A.
Gamma-ray emission up to and above 100 TeV is detected from the supernova remnant G106.3+2.7. The emission above 10 TeV is associated with a molecular cloud rather than the pulsar PSR J2229+6114, favouring a hadronic origin via the π0 decay caused by accelerated relativistic protons.
Tidal disruption events are an excellent probe for supermassive black holes in distant inactive galaxies because they emit bright multi-wavelength flares that last several months to years. AT2019dsg represents the first potential association of neutrino emission with such an explosive event.
The tidal disruption event AT2019dsg is probably associated with a high-energy neutrino, suggesting that such events can contribute to the cosmic neutrino flux. The electromagnetic emission is explained in terms of a central engine, a photosphere and an extended synchrotron-emitting outflow.
A delayed radio flare six months after an optically discovered tidal disruption event, followed by a second and brighter flare, years later, may potentially be due to the delayed ejection of an outflow following a transition in accretion states.
Outbursts from accreting pulsars encode much information on mass accretion in X-ray binary systems. Measuring optical as well as X-ray pulsations can constrain models and, indeed, point to particle acceleration taking place during accretion.
Tidal-evolution modelling, combined with new geophysical constraints of Mars and viscoelastic laboratory measurements, suggests that the two Martian moons have a common progenitor that was disrupted between 1 and 2.7 billion years ago.
A recent association of a tidal disruption event with neutrino emission can be explained by an expanding cocoon from a relativistic jet providing an external target of backscattered X-rays for the production of neutrinos via proton–photon interactions.
In April 2020, the Konus-Wind instrument registered two X-ray bursts temporally coincident with two radio bursts from the Galactic magnetar SGR 1935+2154. The unusual spectral hardness of the X-ray bursts may be an indicator of fast-radio-burst-like radio emission from magnetars.
Twenty-four X-ray bursts from a Galactic magnetar simultaneously observed with NICER and Fermi permit a direct comparison to a later X-ray burst that was coincident with a fast radio burst (FRB). The FRB-related burst is spectrally distinct, pointing to an unusual point of emission.
Insight-HXMT detected a double-peaked X-ray burst from Galactic magnetar SGR J1935+2154, consistent with two fast radio bursts (FRBs) observed from the same object within seconds. This coincidence suggests a common physical origin, and gives insight into the mechanism behind the origin of FRBs.
In April 2020, the AGILE satellite registered an X-ray burst temporally coincident with a radio burst from the Galactic magnetar SGR 1935+2154. As seen in hard X-rays, the burst was cut off above 80 keV and had an isotropically emitted energy of about 1040 erg.