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1. Solitary waves in mass-in-mass lattices

   https://doi.org/10.1007/s00033-020-01384-8  

   Faver, Timothy E.; Goodman, Roy H.; Wright, J. Douglas (December 2020, Zeitschrift für angewandte Mathematik und Physik)

   null (Ed.)
2. Satellite mass functions and the faint end of the galaxy mass–halo mass relation in LCDM

   https://doi.org/10.1093/mnras/stac2057  

   Santos-Santos, Isabel M. E.; Sales, Laura V.; Fattahi, Azadeh; Navarro, Julio F. (July 2022, Monthly Notices of the Royal Astronomical Society)

   ABSTRACT The abundance of the faintest galaxies provides insight into the nature of dark matter and the process of dwarf galaxy formation. In the LCDM scenario, low-mass haloes are so numerous that the efficiency of dwarf formation must decline sharply with decreasing halo mass in order to accommodate the relative scarcity of observed dwarfs and satellites in the Local Group. The nature of this decline contains important clues to the mechanisms regulating the onset of galaxy formation in the faintest systems. We explore here two possible models for the stellar mass (M*)–halo mass (M200) relation at the faint end, motivated by some of the latest LCDM cosmological hydrodynamical simulations. One model includes a sharp mass threshold below which no luminous galaxies form, as expected if galaxy formation proceeds only in systems above the hydrogen-cooling limit. In the second model, M* scales as a steep power law of M200 with no explicit cut-off, as suggested by recent semi-analytical work. Although both models predict satellite numbers around Milky Way-like galaxies consistent with current observations, they predict vastly different numbers of ultrafaint dwarfs and of satellites around isolated dwarf galaxies. Our results illustrate how the satellite mass function around dwarfs may be used to probe the M*–M200 relation at the faint end and to elucidate the mechanisms that determine which low-mass haloes ‘light up’ or remain dark in the LCDM scenario. 

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3. Mass‐in‐mass lattices with small internal resonators

   https://doi.org/10.1111/sapm.12340  

   Hadadifard, Fazel; Wright, J. Douglas (January 2021, Studies in Applied Mathematics)

   null (Ed.)
4. Mass in Kähler Geometry

   https://doi.org/10.1007/s00220-016-2661-4  

   Hein, Hans-Joachim; LeBrun, Claude (October 2016, Communications in Mathematical Physics)

   null (Ed.)
5. Extreme Mass Loss in Low-mass Type Ib/c Supernova Progenitors

   https://doi.org/10.3847/2041-8213/ac9b3d  

   Wu, Samantha_C; Fuller, Jim (November 2022, The Astrophysical Journal Letters)

   Abstract Many core-collapse supernovae (SNe) with hydrogen-poor and low-mass ejecta, such as ultra-stripped SNe and type Ibn SNe, are observed to interact with dense circumstellar material (CSM). These events likely arise from the core collapse of helium stars that have been heavily stripped by a binary companion and have ejected significant mass during the last weeks to years of their lives. In helium star models run to days before core collapse we identify a range of helium core masses ≈2.5–3M_⊙whose envelopes expand substantially due to the helium shell burning while the core undergoes neon and oxygen burning. When modeled in binary systems, the rapid expansion of these helium stars induces extremely high rates of late-stage mass transfer ( $\dot{M}\gtrsim {10}^{-2}{M}_{\odot }{\mathrm{yr}}^{-1}$) beginning weeks to decades before core collapse. We consider two scenarios for producing CSM in these systems: either mass transfer remains stable and mass loss is driven from the system in the vicinity of the accreting companion, or mass transfer becomes unstable and causes a common envelope event (CEE) through which the helium envelope is unbound. The ensuing CSM properties are consistent with the CSM masses (∼10⁻²–1M_⊙) and radii (∼10¹³–10¹⁶cm) inferred for ultra-stripped SNe and several type Ibn SNe. Furthermore, systems that undergo a CEE could produce short-period neutron star binaries that merge in less than 100 Myr. 

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