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Abstract A series of solar energetic electron (SEE) events was observed from 2022 November 9 to November 15 by Solar Orbiter, STEREO-A, and near-Earth spacecraft. At least 32 SEE intensity enhancements at energies >10 keV were clearly distinguishable in Solar Orbiter particle data, with 13 of them occurring on November 11. Several of these events were accompanied by ≲10 MeV proton and ≲2 MeV nucleon⁻¹heavy-ion intensity enhancements. By combining remote-sensing and in situ data from the three viewpoints (Solar Orbiter and STEREO-A were ∼20° and ∼15° east of Earth, respectively), we determine that the origin of this rapid succession of events was a series of brightenings and jetlike eruptions detected in extreme ultraviolet (EUV) observations from the vicinity of two active regions. We find a close association between these EUV phenomena, the occurrence of hard X-ray flares, type III radio bursts, and the release of SEEs. For the most intense events, usually associated with extended EUV jets, the distance between the site of these solar eruptions and the estimated magnetic connectivity regions of each spacecraft with the Sun did not prevent the arrival of electrons at the three locations. The capability of jets to drive coronal fronts does not necessarily imply the observation of an SEE event. Two peculiar SEE events on November 9 and 14, observed only at electron energies ≲50 keV but rich in ≲1 MeV nucleon⁻¹heavy ions, originated from slow-rising confined EUV emissions, for which the process resulting in energetic particle release to interplanetary space is unclear. 

Abstract The HH 24 complex harbors five collimated jets emanating from a small protostellar multiple system. We have carried out a multiwavelength study of the jets, their driving sources, and the cloud core hosting the embedded stellar system, based on data from the Hubble Space Telescope, Gemini, Subaru, Apache Point Observatory 3.5 m, Karl G. Jansky Very Large Array, and Atacama Large Millimeter/submillimeter Array (ALMA) telescopes. The data show that the multiple system, SSV 63, contains at least 7 sources, ranging in mass from the hydrogen-burning limit to proto-Herbig Ae stars. The stars are in an unstable nonhierarchical configuration, and one member, a borderline brown dwarf, is moving away from the protostellar system with 25 km s⁻¹, after being ejected ∼5800 yr ago as an orphaned protostar. Five of the embedded sources are surrounded by small, possibly truncated, disks resolved at 1.3 mm with ALMA. Proper motions and radial velocities imply jet speeds of 200–300 km s⁻¹. The two main HH 24 jets, E and C, form a bipolar jet system that traces the innermost portions of parsec-scale chains of Herbig–Haro and H₂shocks with a total extent of at least 3 pc. H₂CO and C¹⁸O observations show that the core has been churned and continuously fed by an infalling streamer.¹³CO and¹²CO trace compact, low-velocity, cavity walls carved by the jets and an ultracompact molecular outflow from the most embedded object. ChaoticN-body dynamics likely will eject several more of these objects. The ejection of stars from their feeding zones sets their masses. Dynamical decay of nonhierarchical systems can thus be a major contributor to establishing the initial mass function. 

All-organic, heavy-atom-free photosensitizers based on thionation of nucleobases are receiving increased attention because they are easy to make, noncytotoxic, work both in the presence and absence of molecular oxygen and can be readily incorporated into DNA and RNA. In this contribution, the DNA and RNA fluorescent probe, thieno[3,4-d]pyrimidin-4(1H)-one, has been thionated to develop thieno[3,4-d]pyrimidin-4(1H)-thione, which is nonfluorescent and absorbs near-visible radiation with about 60% higher efficiency. Steady-state absorption and emission spectra are combined with transient absorption spectroscopy and CASPT2 calculations to delineate the electronic relaxation mechanisms of both pyrimidine derivatives in aqueous and acetonitrile solutions and to explain the origin of the remarkable fluorescence quenching in the thionated compound. It is demonstrated that thieno[3,4-d]pyrimidin-4(1H)-thione efficiently populates the long-lived and reactive triplet state in hundreds of femtoseconds independent of solvent. Conversely, fluorescence emission in thieno[3,4-d]pyrimidin-4(1H)-one is highly sensitive to solvent, with an order of magnitude decrease in fluorescence yield in going from aqueous to acetonitrile solution. Collectively, the experimental and computational results demonstrate that thieno[3,4-d]pyrimidine-4(1H)-thione stands out as the most promising thiopyrimidine photosensitizer developed to this date, which can be readily incorporated as a photodynamic agent into sequence-specific DNA and RNA sequences for the treatment of skin cancer cells. 

The substitution of an oxygen atom in an exocyclic carbonyl group of the nucleobases by a sulfur atom in a nucleic acid base generates a thiobase. This substitution causes a redshift in the absorption spectrum of the thiobase with respect to the canonical nucleobase, moving the strongly allowed absorption band from the UVC to the UVA region of the electromagnetic spectrum. Due to this redshift and the efficient population of the triplet state, 4-thiothymidine (4tThd) can be selectively excited without exciting canonical DNA, making it a powerful UVA photosensitizer. The synergistic toxicity of 4tThd and UVA radiation allows for the enhanced killing of skin cancer cells. As a result, 4tThd has been proposed for use in conjunction with UVA radiation as potential photodynamic therapy agent, due to its photochemical properties and to a diminished cytotoxicity. Studies of the monomer 4tThd have been performed to explore the prospective use of 4tThd in photochemotherapeutic application with reduced phototoxic side effects. One study of 4tThd in aqueous solution proposed the main kinetic mechanism to consist of intersystem crossing from the S2 state to the triplet manifold. Vertical excitation energies were calculated using the optimized ground state of 4tThd in water and vacuum. These were found to be in good agreement with the values previously reported. After studying the monomer, the next step is to understand what happens when 4tThd interacts with the DNA bases. Therefore, ground state optimizations and vertical excitation energies calculations were performed for a series of 4tThd-containing dinucleotides. These vertical excitation energy calculations predict the order electronic states and likely kinetic mechanisms when 4tThd is incorporated into DNA, which will greatly assist in the interpretation of planned time-resolved experiments. 

In this study we analyze 70 radio continuum sources associated with dust clumps and considered to be candidates for the earliest stages of high-mass star formation. The detection of these sources was reported by Rosero et al. (2016), who found most of them to show weak ( < 1 mJy) and compact ( < 0.6") radio emission. Herein, we used the observed parameters of these sources to investigate the origin of the radio continuum emission. We found that at least ∼ 30% of these radio detections are most likely ionized jets associated with high-mass protostars, but for the most compact sources we cannot discard the scenario that they represent pressure-confined HII regions. This result is highly relevant for recent theoretical models based on core accretion that predict the first stages of ionization from high-mass stars to be in the form of jets. Additionally, we found that properties such as the radio luminosity as a function of the bolometric luminosity of ionized jets from low and high-mass stars are extremely well-correlated. Our data improve upon previous studies by providing further evidence of a common origin for jets independently of luminosity.