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   https://doi.org/10.3847/1538-4357/abc3c2  

   Cheng, Xinlun; Anguiano, Borja; Majewski, Steven R.; Hayes, Christian; Arras, Phil; Chiappini, Cristina; Hasselquist, Sten; de Andrade Queiroz, Anna Bárbara; Nitschelm, Christian; García-Hernández, Domingo Aníbal; et al (December 2020, The Astrophysical Journal)
2. LISA Galactic binaries in the Roman Galactic Bulge Time-Domain Survey

   https://doi.org/10.1093/mnras/stad2290  

   Digman, Matthew C; Hirata, Christopher M (August 2023, Monthly Notices of the Royal Astronomical Society)

   ABSTRACT Short-period Galactic white dwarf binaries detectable by Laser Interferometer Space Antenna are the only guaranteed persistent sources for multimessenger gravitational-wave astronomy. Large-scale surveys in the 2020s present an opportunity to conduct preparatory science campaigns to maximize the science yield from future multimessenger targets. The Nancy Grace Roman Space Telescope Galactic Bulge Time-Domain Survey will (in its Reference Survey design) image seven fields in the Galactic Bulge approximately 40 000 times each. Although the Reference Survey cadence is optimized for detecting exoplanets via microlensing, it is also capable of detecting short-period white dwarf binaries. In this paper, we present forecasts for the number of detached short-period binaries the Roman Galactic Bulge Time-Domain Survey will discover and the implications for the design of electromagnetic surveys. Although population models are highly uncertain, we find a high probability that the baseline survey will detect of the order of ∼5 detached white dwarf binaries. The Reference Survey would also have a $${\gtrsim} 20\,{\rm per\,cent}$$ chance of detecting several known benchmark white dwarf binaries at the distance of the Galactic Bulge. 

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3. How supernovae launch galactic winds?

   https://doi.org/10.1093/mnrasl/slx072  

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4. Modeling Turbulence in Galactic Centers

   https://doi.org/10.3847/1538-3881/abefd3  

   Salas, Jesus M.; Morris, Mark R.; Naoz, Smadar (April 2021, The Astronomical Journal)

   null (Ed.)
5. Galactic Positrons from Thermonuclear Supernovae

   https://doi.org/10.3847/1538-4357/ac5253  

   Mera Evans, T. B.; Hoeflich, P.; Diehl, R. (May 2022, The Astrophysical Journal)

   Abstract Type Ia supernovae (SNe Ia) may originate from a wide variety of explosion scenarios and progenitor channels. They exhibit a factor of ≈10 difference in brightness and thus a differentiation in the mass of 56 Ni → 56 Co → 56 Fe. We present a study on the fate of positrons within SNe Ia in order to evaluate their escape fractions and energy spectra. Our detailed Monte Carlo transport simulations for positrons and γ -rays include both β + decay of 56 Co and pair production. We simulate a wide variety of explosion scenarios, including the explosion of white dwarfs (WDs) close to the Chandrasekhar mass ( M Ch ), He-triggered explosions of sub- M Ch WDs, and dynamical mergers of two WDs. For each model, we study the influence of the size and morphology of the progenitor magnetic field between 1 and 10 13 G. Population synthesis based on the observed brightness distribution of SNe Ia was used to estimate the overall contributions to Galactic positrons due to escape from SNe Ia. We find that this is dominated by SNe Ia of normal brightness, where variations in the distribution of emitted positrons are small. We estimate a total SNe Ia contribution to Galactic positrons of <2% and, depending on the magnetic field morphology, <6–20% for M Ch and sub- M Ch , respectively. 

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