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1. Type-II WS ₂ –ReSe ₂ heterostructure and its charge-transfer properties

   https://doi.org/10.1557/jmr.2019.374  

   Han, Xiuxiu ; He, Dawei ; Zhang, Lu ; Hao, Shengcai ; Liu, Shuangyan ; Fu, Jialu ; Miao, Qing ; He, Jiaqi ; Wang, Yongsheng ; Zhao, Hui ( June 2020 , Journal of Materials Research)

   We fabricated a van der Waals heterostructure of WS 2 –ReSe 2 and studied its charge-transfer properties. Monolayers of WS 2 and ReSe 2 were obtained by mechanical exfoliation and chemical vapor deposition, respectively. The heterostructure sample was fabricated by transferring the WS 2 monolayer on top of ReSe 2 by a dry transfer process. Photoluminescence quenching was observed in the heterostructure, indicating efficient interlayer charge transfer. Transient absorption measurements show that holes can efficiently transfer from WS 2 to ReSe 2 on an ultrafast timescale. Meanwhile, electron transfer from ReSe 2 to WS 2 was also observed. The charge-transfer properties show that monolayers of ReSe 2 and WS 2 form a type-II band alignment, instead of type-I as predicted by theory. The type-II alignment is further confirmed by the observation of extended photocarrier lifetimes in the heterostructure. These results provide useful information for developing van der Waals heterostructure involving ReSe 2 for novel electronic and optoelectronic applications and introduce ReSe 2 to the family of two-dimensional materials to construct van der Waals heterostructures.
2. Visible and near-infrared spectro-interferometric analysis of the edge-on Be star o Aquarii

   https://doi.org/10.1051/0004-6361/201936039  

   de Almeida, E. S. ; Meilland, A. ; Domiciano de Souza, A. ; Stee, P. ; Mourard, D. ; Nardetto, N. ; Ligi, R. ; Tallon-Bosc, I. ; Faes, D. M. ; Carciofi, A. C. ; et al ( April 2020 , Astronomy & Astrophysics)

   Aims. We present a detailed visible and near-infrared spectro-interferometric analysis of the Be-shell star o Aquarii from quasi-contemporaneous CHARA/VEGA and VLTI/AMBER observations. Methods. We analyzed spectro-interferometric data in the H α (VEGA) and Br γ (AMBER) lines using models of increasing complexity: simple geometric models, kinematic models, and radiative transfer models computed with the 3D non-LTE code HDUST. Results. We measured the stellar radius of o Aquarii in the visible with a precision of 8%: 4.0 ± 0.3 R ⊙ . We constrained the circumstellar disk geometry and kinematics using a kinematic model and a MCMC fitting procedure. The emitting disk sizes in the H α and Br γ lines were found to be similar, at ~10–12 stellar diameters, which is uncommon since most results for Be stars indicate a larger extension in H α than in Br γ . We found that the inclination angle i derived from H α is significantly lower (~15°) than the one derived from Br γ : i ~ 61.2° and 75.9°, respectively. While the two lines originate from a similar region of the disk, the disk kinematics were found to be near to the Keplerian rotation (i.e., β = −0.5) in Br γmore »( β ~ −0.43), but not in H α ( β ~ −0.30). After analyzing all our data using a grid of HDUST models (BeAtlas), we found a common physical description for the circumstellar disk in both lines: a base disk surface density Σ 0 = 0.12 g cm −2 and a radial density law exponent m = 3.0. The same kind of discrepancy, as with the kinematic model, is found in the determination of i using the BeAtlas grid. The stellar rotational rate was found to be very close (~96%) to the critical value. Despite being derived purely from the fit to interferometric data, our best-fit HDUST model provides a very reasonable match to non-interferometric observables of o Aquarii: the observed spectral energy distribution, H α and Br γ line profiles, and polarimetric quantities. Finally, our analysis of multi-epoch H α profiles and imaging polarimetry indicates that the disk structure has been (globally) stable for at least 20 yr. Conclusions. Looking at the visible continuum and Br γ emission line only, o Aquarii fits in the global scheme of Be stars and their circumstellar disk: a (nearly) Keplerian rotating disk well described by the viscous decretion disk (VDD) model. However, the data in the H α line shows a substantially different picture that cannot fully be understood using the current generation of physical models of Be star disks. The Be star o Aquarii presents a stable disk (close to the steady-state), but, as in previous analyses, the measured m is lower than the standard value in the VDD model for the steady-state regime ( m = 3.5). This suggests that some assumptions of this model should be reconsidered. Also, such long-term disk stability could be understood in terms of the high rotational rate that we measured for this star, the rate being a main source for the mass injection in the disk. Our results on the stellar rotation and disk stability are consistent with results in the literature showing that late-type Be stars are more likely to be fast rotators and have stable disks.« less
3. Spectropolarimetry of the Type Ia SN 2019ein rules out significant global asphericity of the ejecta

   https://doi.org/10.1093/mnras/stab3136  

   Patra, Kishore C ; Yang ; Brink, Thomas G ; Höflich, Peter ; Wang, Lifan ; Filippenko, Alexei V ; Kasen, Daniel ; Baade, Dietrich ; Foley, Ryan J ; Maund, Justyn R ; et al ( December 2021 , Monthly Notices of the Royal Astronomical Society)

   ABSTRACT Detailed spectropolarimetric studies may hold the key to probing the explosion mechanisms and the progenitor scenarios of Type Ia supernovae (SNe Ia). We present multi-epoch spectropolarimetry and imaging polarimetry of SN 2019ein, an SN Ia showing high expansion velocities at early phases. The spectropolarimetry sequence spans from ∼−11 to +10 d relative to peak brightness in the B band. We find that the level of the continuum polarization of SN 2019ein, after subtracting estimated interstellar polarization, is in the range 0.0–0.3 per cent, typical for SNe Ia. The polarization position angle remains roughly constant before and after the SN light-curve peak, implying that the inner regions share the same axisymmetry as the outer layers. We observe high polarization (∼1 per cent) across both the Si ii λ6355 and Ca ii near-infrared triplet features. These two lines also display complex polarization modulations. The spectropolarimetric properties of SN 2019ein rule out a significant departure from spherical symmetry of the ejecta for up to a month after the explosion. These observations disfavour merger-induced and double-detonation models for SN 2019ein. The imaging polarimetry shows weak evidence for a modest increase in polarization after ∼20 d since the B-band maximum. If this rise is real and is observed in other SNe Ia at similar phases, we may havemore »seen, for the first time, an aspherical interior similar to what has been previously observed for SNe IIP. Future polarization observations of SNe Ia extending to post-peak epochs will help to examine the inner structure of the explosion.« less
4. The 3D shape of Type IIb SN 2011hs

   https://doi.org/https://ui.adsabs.harvard.edu/link_gateway/2019MNRAS.485..102S/doi:10.1093/mnras/stz265  

   H. F. Stevance1?, J.R. Maund1y ( July 2019 , Monthly notices of the Astronomical Society of London)

   We observed seven epochs of spectropolarimetry in optical wavelengths for the Type IIb SN 2011hs, ranging from 􀀀3 to +40 days with respect to V -band maximum. A high degree of interstellar polarization was detected (up to 3 percent), with a peak lying blueward of 4500A. Similar behaviours have been seen in some Type Ia SNe, but had never been observed in a Type IIb. We nd that it is most likely the result of a relative enhancement of small silicate grains in the vicinity of the SN. Signi cant intrinsic continuum polarization was recovered at 􀀀3 and +2 days (p = 0.55  0.12 percent and p = 0.75  0.11 percent, respectively). We discuss the change of the polarization angle across spectral lines and in the continuum as diagnostics for the 3D structure of the ejecta. We see a gradual rotation by about 􀀀50 in the continuum polarization angle between 􀀀2 and +18 days after V -band maximum. A similar rotation in He i 5876, H and the Ca ii infrared triplet seems to indicate a strong in uence of the global geometry on the line polarization features. The di erences in the evolution of their respective loopsmore »on the Stokes q 􀀀 u plane suggest that line speci c geometries are also being probed. Possible interpretations are discussed and placed in the context of literature. We nd that the spectropolarimetry of SN 2011hs is most similar to that of SN 2011dh, albeit with notable di erences.« less
5. The Magellanic Edges Survey – III. Kinematics of the disturbed LMC outskirts

   https://doi.org/10.1093/mnras/stac733  

   Cullinane, L. R. ; Mackey, A. D. ; Da Costa, G. S. ; Erkal, D. ; Koposov, S. E. ; Belokurov, V. ( March 2022 , Monthly Notices of the Royal Astronomical Society)

   We explore the structural and kinematic properties of the outskirts of the Large Magellanic Cloud (LMC) using data from the Magellanic Edges Survey (MagES) and Gaia EDR3. Even at large galactocentric radii (8° < R < 11°), we find the north-eastern LMC disc is relatively unperturbed: its kinematics are consistent with a disc of inclination ∼36.5° and line-of-nodes position angle ∼145° east of north. In contrast, fields at similar radii in the southern and western disc are significantly perturbed from equilibrium, with non-zero radial and vertical velocities, and distances significantly in front of the disc plane implied by our north-eastern fields. We compare our observations to simple dynamical models of the Magellanic or Milky Way system which describe the LMC as a collection of tracer particles within a rigid potential, and the Small Magellanic Cloud (SMC) as a rigid Hernquist potential. A possible SMC crossing of the LMC disc plane ∼400 Myr ago, in combination with the LMC’s infall to the Milky Way potential, can qualitatively explain many of the perturbations in the outer disc. Additionally, we find the claw-like and arm-like structures south of the LMC have similar metallicities to the outer LMC disc ([Fe/H] ∼ −1), and aremore »likely comprised of perturbed LMC disc material. The claw-like substructure is particularly disturbed, with out-of-plane velocities >60 km s−1 and apparent counter-rotation relative to the LMC’s disc motion. More detailed N-body models are necessary to elucidate the origin of these southern features, potentially requiring repeated interactions with the SMC prior to ∼1 Gyr ago.

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