Abstract The parameter space for mass loss in Type Ia supernova (SN Ia) progenitors is large, with different progenitor scenarios favoring different mass-loss regimes. Here we focus on the impact that uniform and isotropic outflows have on the circumstellar environment of SN Ia progenitors. We vary mass-loss rate, wind velocity, and outflow duration, and evolve supernova remnant (SNR) models in this grid of circumstellar structures in order to compare the bulk properties of these models (ages, radii, and Fe K α centroids and luminosities) to observations. We find that roughly 55% (7/13) of young X-ray-bright Type Ia SNRs in the Milky Way and the Large Magellanic Cloud had progenitors that did not substantially modify their surroundings on ∼parsec scales. This group includes SN Ia with a range of luminosities, and at least one likely product of a double-detonation explosion in a sub-Chandrasekhar white dwarf (WD). The other half of our sample can be divided into two distinct classes. A small subset of SNRs (∼15%, 2/13) have large radii and low Fe K α centroids and are likely expanding into large cavities that might have been excavated by fast (∼1000 km s −1 ), sustained progenitor outflows. The majority of the SNRs that are expanding into a modified medium (∼30%, 4/13) show evidence for dense material, likely associated with slow (∼10 km s −1 ) progenitor outflows, possibly a byproduct of accretion processes in near-Chandrasekhar WDs spawned by younger stellar populations.

Abstract Early-time spectroscopy of supernovae (SNe), acquired within days of explosion, yields crucial insights into their outermost ejecta layers, facilitating the study of their environments, progenitor systems, and explosion mechanisms. Recent efforts in early discovery and follow-up of SNe have shown the potential insights that can be gained from early-time spectra. Surveys such as the Time-Domain Extragalactic Survey (TiDES), conducted with the 4-meter Multi-Object Spectroscopic Telescope (4MOST), will provide spectroscopic follow-up of transients discovered by the Legacy Survey of Space and Time (LSST). Current simulations indicate that early-time spectroscopic studies conducted with TiDES data will be limited by the current SN selection criteria. To enhance early-time SN spectroscopic studies from TiDES-like surveys, we propose a set of selection criteria focusing on young SNe (YSNe), which we define as SNe prior to −10 days before peak brightness. Utilising the Zwicky Transient Facility transient alerts, we developed criteria to select YSNe while minimising the sample’s contamination rate to 23percnt. The developed criteria were applied to LSST simulations, yielding a sample of 694 Deep Drilling Field survey SNe and 56260 Wide Fast Deep survey SNe for follow-up. We demonstrate that our criteria enables the selection of SNe at early-times, enhancing future early-time spectroscopic SN studies from TiDES-like surveys. Finally, we investigated 4MOST-like observing strategies to increase the sample of spectroscopically observed YSNe. We propose that a 4MOST-like observing strategy that follows LSST with a delay of 3 days is optimal for a TiDES-like SN survey in terms of the number of classifiable spectra obtained, while a 1 day delay is most optimal for enhancing the early-time science in conjunction with our YSN selection criteria.

Abstract The life-cycle, structure, and dynamics of the interstellar medium (ISM) is regulated by turbulence. Complex physical processes, including supernova (SN) explosions, shear, and gravitational collapse, drive and maintain turbulence, but it is still an open question what turbulence driving mode is primarily excited by these different mechanisms. The turbulence driving parameter, b, can be used to quantify the ratio of solenoidal to compressive modes in the acceleration field that drives the turbulence. Compressive driving is characterised by b ∼ 1, while purely solenoidal driving gives b ∼ 0.3. To quantify the turbulence in the galactic ISM, we investigate the time evolution of b, as well as the turbulent Mach number, and plasma β (thermal-to-magnetic pressure ratio), and its correlation with star formation in the magnetised warm neutral medium (WNM) of the TIGRESS shearing-box simulations of a ∼ kpc-sized patch of a Milky-Way-like galaxy, over a 100 Myr time period (∼ half an orbital time). In this simulation the turbulence is driven by a combination of shear, gravitational collapse, and star formation feedback in the form of radiation and SNe. We find that the turbulence driving parameter fluctuates in time between b ∼ 0.4 and b ∼ 1. We find a time-dependent correlation of b with star formation activity, such that high star formation rates follow about one turbulent turnover time (∼10 Myr) after phases of highly compressive driving (b > 0.5). About 20 Myr after the peak in star formation, type-B SN feedback drives up the WNM fraction and turbulent Mach numbers, and reduces plasma β and the driving to b ∼ 0.4 − 0.5.

Abstract We develop a new statistical framework for studying the host galaxies of astrophysical sources that accounts for both redshift evolution and the multivariate nature of the properties of host galaxies. These aspects are critical when dealing with sources that span a wide range of redshifts, and/or with unknown redshift-dependent selection effects. We apply our method to a sample of fast radio burst (FRB) host galaxies as a means of probing the uncertain progenitor(s) of these events. Using our method, we are able to rule out that FRBs track star formation rate (SFR), as would be expected if FRBs are associated exclusively with young neutron stars born via core-collapse supernovae (SNe). Furthermore, we rule out a recently proposed metallicity-dependent model whereby FRBs track SFR only above an oxygen abundance of 12 + log ( O / H ) ∼ 8 . Motivated by the fact that at least one FRB has been localized to a globular cluster (GC), we also investigate the hypothesis that FRB sources track GC mass and explicitly rule out this scenario. Alternatively, we find that a “mixed” model, whereby FRBs track a linear combination of SFR and stellar mass, best explains the data. The preferred parameters of such a mixed model are similar to those inferred for Type Ia SNe and imply a possible connection between the progenitors of these different transients.

Supernova (SN) feedback-driven galactic outflows are a key physical process that contributes to the baryon cycle by regulating star formation activity, reducing the amount of metals in low-mass galaxies and enriching the circumgalactic (CGM) and intergalactic media (IGM). We aim to understand the chemical loop of sub-Milky Way (MW) galaxies and their nearby regions. We studied 15 simulated central sub-MW galaxies (mstar łeq 10^ 10 and intermediate-mass galaxies (mstar ∼ 10 10 $ Msun) from the CIELO-P7 high-resolution simulations. We followed the evolution of the progenitor galaxies, their properties, and the characteristics of the outflows within the redshift range $z = 0, 7 . We used two dynamically motivated outflow definitions, unbound outflows, and expelled mass rates to quantify the impact of SN feedback. At z ∼ 0, sub-MW galaxies have a larger fraction of their current oxygen mass in the gas phase but have expelled a greater portion beyond the virial radius, compared to their higher-mass counterparts. Galaxies with M_ * < ∼ 10^ 9 have 10–40 percent of their total oxygen mass within ̊vir in the CGM and an equivalent to 10–60 percent expelled into the IGM. In contrast, more massive galaxies have most of their oxygen mass locked by the stellar populations. The CGM of low-mass galaxies predominantly contains oxygen low-temperature gas, which acts as a metal reservoir. We find that the outflows are more oxygen-rich for sub-MW galaxies, ̊m Z_ ̊m out /Z_ ISM ∼ 1.5, than for higher-mass galaxies, ̊m Z_ ̊m out /Z_ ISM łeq 0.5, particularly for z <2. Mass-loading factors of ̊m η_ out are detected, in agreement with observations. While a weak dependence of η on mass and circular velocity is found at z∼ 0, a stronger anti-correlation appears for higher redshift. Our results suggest that sub-MW galaxies may store a significant fraction of metals in their CGM and that the anti-correlation between η and stellar mass (or circular velocity) is stronger at z ∼ 2, which is likely due to a combination of more intense star formation, a higher merger rate, and shallower potential wells.

Stripped-envelope supernovae (SESNe), including Type IIb, Ib, and Ic supernovae (SNe), originate from the explosions of massive stars whose outer envelopes have been largely removed during their lifetimes. The main stripping mechanism for the hydrogen (H) envelope in the progenitors of SESNe is often considered to be interaction with a binary companion, but the stripping mechanism for the helium (He) layer is unclear. We study the process of the He-layer stripping in the progenitors of SESNe. This is closely related to the origin of their diverse observational properties. We conducted photometric and spectroscopic observations of the Type Ib SN 2021efd, which shows signs of interaction with H-free circumstellar material (CSM). At early phases, its photometric and spectroscopic properties resemble those of typical Type Ib SNe. Around 30 days after the r-band light curve (LC) peak until at least ∼ 770 days, the luminosity of the multiband LCs is higher than that of regular SESNe and has at least three distinct peaks. The LC evolution is similar to that of SN 2019tsf, whose previously unpublished spectrum at 400 days is also presented here. The nebular spectrum of SN 2021efd shows narrow emission lines (sim1000 km s -1 ) in various species, such as O i , , , , Ca ii Mg ii He i O i , Ca ii , and S ii . Based on the observations, we studied the properties of the ejecta and CSM of SN 2021efd. Our observations suggest that SN 2021efd is a Type Ib SN that interacts with the CSM with the following parameters: The estimated ejecta mass, explosion energy, and 56 Ni mass are 2.2 M_⊙$, 9.1 50 erg , and 0.14 M_⊙, respectively, and the estimated CSM mass, composition, and distribution are at least a few times 0.1 M$_⊙, H free, and clumpy, respectively. Based on the estimated ejecta properties, we conclude that this event is a transitional SN whose progenitor was experiencing He-layer stripping at the epoch of the explosion and was on the way to becoming a carbon-oxygen star (as the progenitors of Type Ic SNe) from a He star (as the progenitors of Type Ib SNe). The estimated CSM properties suggest that the progenitor had some episodic mass ejections at a rate of ∼ 5 -10^ 10^ -3 -2 M_⊙ ^ yr -1 for the last decade and slightly lower before this final phase at least from sim200 years before the explosion for the assumed CSM velocity of 100 km s -1 $. For the case of ∼ 1000 km s$^ -1 , the necessary mass-loss rate would be higher by a factor of ten, and the timescales would be shorter by a factor of ten.

Abstract The Shanghai Jiao Tong University Spectroscopic Telescope(JUST) holds significant importance for astronomy in China. It will assist scientists in achieving a series of influential research results in fields such as supernova explosions, identification of gravitational wave sources, and exoplanet detection with its outstanding sky survey capability and high-precision observation technology. The 4.4-meter primary mirror of JUST will adopt segmented mirror active optics technology,which could be divided into two cases: the segmented primary mirror will be in co-focus under the limit of seeing;it will be equipped with adaptive optics, and the segmented primary mirror will achieve co-phasing in the near-infrared waveband(such as 1.8 µm). This paper will focus on the research of errors of the hexagonal segments in the primary mirror under the two conditions. Additionally, separate and comprehensive error simulations were conducted, obtaining a large number of successful simulation results.

Supernovae (SNe), the catastrophic end of stars’ lives, are among the most energetic phenomena in the universe. Mapping the aftermath of the explosions to the properties of pre-SN stars is challenging due to the lack of knowledge about the evolution of different types of stars. The immediate surroundings of pre-SN stars carry the signature of the progenitors, and radio observations are the best way to examine the ambient media. Since radio emission originates from the interaction of supersonic SN ejecta with the relatively stationary circumstellar medium, with a few years of radio study, the mass-loss history of progenitor stars can be probed from just before the explosion of the star to thousands of years before the onset of the SN. Moreover, this can provide crucial details about the explosions, which are poorly understood to date. In this paper, we review the radio properties of different types of core-collapse explosions and thermonuclear runaways to understand their mass-loss evolution—which allows us to unravel the imprints of the progenitors on the surrounding media and thus the nature of the exploded stars. Additionally, we discuss the current state of the art in this field, including existing and the next-generation radio facilities with enhanced capabilities that provide further details about these explosions.

Accurate cosmological constraints from type Ia supernovae (SNe) require sufficiently accurate corrections for host-galaxy extinction. Modelling these corrections is challenged by the problem of disentangling the SN's intrinsic colours from host-galaxy interstellar reddening. The latter is commonly modelled in a probabilistic way assuming an exponential distribution exp(-E(B-V)/τ) as a universal prior, applied across all types of SN host galaxies. We tested the robustness of the exponential model of host-galaxy reddening and its universality against predictions based on simulating dust and type Ia SN distributions in host galaxies of different morphological types. Our simulations incorporated up-to-date observational constraints on dust masses across host-galaxy morphological types, scaling relations between the dust and stellar disc parameters, and the SN distribution. We find substantial differences between predicted interstellar reddening in late- (LT) and early-type (ET) host galaxies, primarily driven by the stellar-to-dust mass ratios. The mean simulated reddening in LT galaxies matches those derived from type Ia SN observations well, but it is significantly lower for ET host galaxies. The obtained reddening distributions exhibit an excess of sight lines with zero reddening with respect to the commonly used exponential model, although the difference is quite mild for LT galaxies. On the other hand, the distribution could peak at E(B-V)>0 when considering a population of young type Ia SNe originating from lower heights within the dust disc of spiral galaxies. The reddening distribution strongly depends on the SN host-galaxy morphological type. Assuming a universal reddening prior distribution for modelling the peak magnitude-colour relation, which is currently a common practice, gives rise to a spurious scatter in the derived extinction properties. It could also bias relative distances between SNe originating from different host-galaxy populations. The discrepancy between the simulated reddening in average ET host galaxies and the observed occurrence of reddened SNe in these galaxies suggests that reddening does not originate from the interstellar dust expected in these hosts.

Abstract We investigate the evolution of red supergiant (RSG) progenitors of core-collapse supernovae (SNe) with initial masses between 12 and 20 M ⊙ , focusing on the effects of enhanced mass loss due to pulsation-driven instabilities in their envelopes and subsequent dynamical ejections during advanced stages of nuclear burning. Using time-dependent mass loss from detailed Modules for Experiments in Stellar Astrophysics (MESA) stellar evolution models, including a parameterized prescription for pulsation-driven superwinds and time-averaged mass-loss rates attributed to resulting shock-induced ejections, we construct the circumstellar medium (CSM) before the SN explosion. We calculate resulting CSM density profiles and column densities considering the acceleration of the stellar wind. Our models produce episodes of enhanced mass loss (∼10 −4 –10 −2 M ⊙ yr −1 ) in the last centuries—decades before explosion forming dense CSM (≳10 −15 g cm −3 at distances ≲10 15 cm)—consistent with those inferred from multiwavelength observations of Type II SNe such as SN 2023ixf, SN 2020ywx, SN 2017hcc, SN 2005ip, and SN 1998S. The formation of such dense circumstellar shells, within the explored range of our single star RSG models, provides a natural explanation for observed flash-ionization signatures, X-ray and radio emission, and has important implications for dust formation around Type II SNe.

Abstract Helium white dwarfs (WDs) with masses less than 0.3 M ⊙ are known as extremely low-mass WDs (ELM WDs), which cannot be produced by single stellar evolution in theory. Generally, these stars are believed to form through binary interactions. Recently, two ELM WDs in unusually wide orbits were reported, i.e., KIC 8145411 and HE 0430-2457. Their orbital separations are too wide to be produced by the binary evolution scenario. In this work, we study the formation of wide-orbit ELM WD binaries from hierarchical triple systems. In this scenario, an ELM WD is formed from the inner binary and subsequently forms a wide binary system with the third object. We find that the merger of an evolved star with a brown dwarf in the inner binary fails to produce single ELM WDs, but Type Ia supernovae (SNe Ia) explosions can successfully do so. Furthermore, we investigate the impact of the supernova explosion on the orbital distribution of the surviving binary and find that this channel may have a probability of reproducing the orbital parameters of HE 0430-2457, but fails to reproduce the observed features of KIC 8145411. This supports recent observational recalibrations suggesting that KIC 8145411 resides in a triple system rather than a binary.

While supernova remnants (SNRs) have been observed to produce up to of dust, the amount of dust destroyed by the forward shock is poorly constrained, raising the question of whether they are net dust producers or destroyers. 1 M_⊙ Our aim was to estimate the dust destruction efficiency of SNR forward shocks in a realistically turbulent interstellar medium (ISM) during their most destructive phase, and to assess dust shielding by high-density filaments during this period. We ran 3D high-resolution turbulence simulations for different turbulent Mach numbers (0--3) and average ISM densities ( ) to resemble observations of the turbulent ISM. We then set off a supernova explosion to trace its 3D magnetohydrodynamic evolution for the first . Finally, we ran post-processing simulations to investigate the dust transport and destruction by the SNR forward shock, taking into account gas and plasma drag, kinetic and thermal sputtering, and grain-grain collisions, and considering either silicates or carbonaceous dust. 1--100 cm -3 10 kyr The dust destruction rate of the forward shock strongly depends on the average ISM density and turbulence strength, varying in the range 27--92% ( ) in the studied . Overall, dust is less efficiently destroyed in a low-density medium (unit 0.85--11.0 M_⊙ 10 kyr 1 cm^ -3 , 27--57%) than in intermediate-density (unit 10 cm^ -3 , 46--92%) and high-density (unit 100 cm^ -3 , 73--87%) cases. The forward shock is found to destroy 8--34% less dust in high Mach turbulence compared to a homogeneous medium. Furthermore, carbonaceous grains are up to 21% more robust than silicates. Filaments can partly shield dust from destruction in the first ; however, always more than of dust is destroyed, making most SNRs dust sinks under the conditions explored in this work. The destruction efficiency of the SNRs with less than of destroyed dust has not yet plateaued, so that they are most likely also net dust destroyers by the end of their lifetimes. 10 kyr 0.85 M_⊙ 1 M_⊙

Abstract We investigate the variability of the UV luminosity function (UVLF) at z > 5 using the SPICE suite of cosmological, radiation-hydrodynamic simulations, which include three distinct supernova (SN) feedback models: bursty-sn, smooth-sn, and hyper-sn. The bursty-sn model, driven by intense and episodic SN explosions, produces the highest fluctuations in the star formation rate (SFR). Conversely, the smooth-sn model, characterized by gentler SN feedback, results in minimal SFR variability. The hyper-sn model, featuring a more realistic prescription that incorporates hypernova (HN) explosions, exhibits intermediate variability, closely aligning with the smooth-sn trend at lower redshifts. These fluctuations in SFR significantly affect the $\rm {{\it M}_{UV} - {\it M}_{halo}}$ relation, a proxy for UVLF variability. Among the models, bursty-sn produces the highest UVLF variability, with a maximum value of 2.5. In contrast, the smooth-sn and hyper-sn models show substantially lower variability, with maximum values of 1.3 and 1.5, respectively. However, in all cases, UVLF variability strongly correlates with host halo mass, with lower-mass halos showing greater variability due to more effective SN feedback in their shallower gravitational wells. The bursty-sn model, though, results in higher amplitudes. Variability decreases in lower mass haloes with decreasing redshift for all feedback models. This study underscores the critical role of SN feedback in shaping the UVLF, and highlights the mass and redshift dependence of its variability, suggesting that UVLF variability may alleviate the bright galaxy tension observed by JWST at high redshifts.

Abstract It is generally believed that the electron-capture reactions happen when the oxygen-neon (ONe) cores grow in masses close to the Chandrasekhar limit, leading to the formation of neutron stars (NSs) via electron-capture supernovae (EC-SNe). EC-SNe are predicted to be the most likely short-lived and faint optical transients, and a small ejecta mass is expected during the collapse. This kind of SNe provide a distinct channel for producing isolated NSs and NS systems, especially for the formation of X-ray binaries and double NSs. However, there are still some uncertainties for the origin of EC-SNe. In this article, we review recent studies on the two classic progenitor channels of EC-SNe, i.e., the single star channel and the binary channel. In the single star channel, EC-SNe can happen in super asymptotic giant branch stars or He stars, whereas in the binary channel EC-SNe can occur in He stars in binaries (including He star+MS systems and NS+He star systems) or accretion-induced collapse in white dwarf binaries (including the single-degenerate scenario and the double-degenerate scenario). Recent progress on the two progenitor channels is discussed, including the initial parameter range for EC-SNe, the evolutionary paths to EC-SNe, related objects, and some observational constraints, etc. We also discuss the impacts of EC-SNe on some research fields, e.g., the properties of NSs, double NSs, chemical products, and some peculiar SNe or events, etc. It is noting that EC-SNe show some similar properties with ultra-stripped SNe, e.g., low ejecta masses and low kicks. Accordingly, we also discuss the difference between these two types of SNe in this article. Research on EC-SNe is at a pivotal stage, with key theoretical uncertainties and observational challenges requiring integrated modeling and multi-wavelength observations for robust identification.

Abstract The abundance patterns of extremely metal-poor stars preserve a fossil record of the Universe’s earliest chemical enrichment by the supernova explosions from the evolution of first generation of stars, also referred to as Population III stars. By applying Bayesian inference to the analysis of abundance patterns of these ancient stars, this study presents a systematic investigation into the properties and explosion mechanism of Pop III stars. We apply NLTE corrections to enhance the reliability of abundance measurements, which significantly reduces the discrepancies in abundances between observations and theoretical yields for odd-Z elements, such as Na and Al. Our Bayesian framework also enables the incorporation of explodability and effectively mitigates biases introduced by varying resolutions across different supernova model grids. In addition to confirming a top-heavy ( α = 0.54) initial mass function for massive Pop III stars, we derive a robust mass–energy relation ( E ∝ M 2 ) of the first supernovae. These findings demonstrate that stellar abundance analysis provides a powerful and independent approach for probing early supernova physics and the fundamental nature of the first stars.

Abstract Shell burning and internal mixing in massive stars play an important role in setting the initial conditions for core-collapse supernova explosions. In the late stages of stellar evolution, intense shell burning can cause distinct convective regions to merge, fundamentally restructuring the stellar interior. Although such phenomena are difficult to observe directly, the observation of “Mg-rich” supernova remnants (SNRs) has recently emerged as a potential signature of these events. In this study, we reanalyze X-ray observations of J0550–6823, a SNR in the Large Magellanic Cloud (LMC) and a new candidate Mg-rich SNR. Our spectral analysis confirms a low Ne/Mg mass ratio of ≈1 and its classification as Mg-rich. By comparing the observational results with presupernova models, we suggest that the progenitor of J0550−6823 likely had an extended convective shell that reduces the Ne/Mg ratio prior to its explosion. Furthermore, we observe that ∼2–3 Mg-rich SNRs exist in the LMC, suggesting that ≲10%–40% of massive stars in the LMC may have had an extended convective shell, similar to what we observed in J0550−6823. This fraction would be important for understanding the final stages of the evolution of massive stars and Galactic chemical evolution.

Abstract Among more than 1000 known fast radio bursts (FRBs), only five sources – FRBs 20121102A, 20190520B, 20201124A, 20240114A and 20190417A – have confirmed associations with persistent radio sources (PRS). The observed quasi-steady emission is consistent with synchrotron radiation from a composite of magnetar wind nebula (MWN) and supernova (SN) ejecta. Using a phenomenological model that incorporates simplified treatments of the nebular dynamics and particle acceleration, we compute the synchrotron flux by solving kinetic equations for energized electrons, accounting for electromagnetic cascades of electron-positron pairs interacting with nebular photons. Within the framework of our model, the rotation-powered scenario requires a young neutron star (NS) with age tage ≈ 20 yr, dipolar magnetic field Bdip ≈ (3 − 5) × 1012 G and initial spin period Pi ≈ 1.5 − 3 ms in an ultra-stripped SN progenitor to account for emissions from FRBs 20121102A and 20190520B. In contrast, FRB 20201124A requires tage ≈ 10 yr, Bdip ≈ 5.5 × 1013 G and Pi ≈ 10 ms in a conventional core-collapse SN progenitor. For the magnetar-flare-powered model, NS aged tage ≈ 25 /40 yr in a USSN progenitor and tage ≈ 12.5 yr in a CCSN progenitor explains the observed flux for FRB 20121102A/20190520B and FRB 20201124A, respectively. Finally, we estimate a minimum NS age tage, min ∼ 1 − 3 yr based on the near-source plasma contribution to observed DM, and tage, min ∼ 6.5 − 10 yr from the absence of radio signal attenuation.

Abstract White dwarfs (WDs) are frequently observed to have strong magnetic fields up to 10 9 G and expected to have a possible internal field as high as ∼10 14 G. High internal fields can significantly deform a WD’s equilibrium structure, generating a quadrupole moment. If the rotation axis is misaligned with the magnetic axis, the deformation can lead to the emission of continuous gravitational waves (CGWs). We examine the potential for detecting CGWs from magnetized WDs with future space-based detectors such as LISA, ALIA, DECIGO, Deci-Hz, the Big Bang Observer, and TianQin. We model the field-induced deformation and compute the resulting GW strain, incorporating amplitude decay due to angular momentum loss from electromagnetic and gravitational radiation. This sets a timescale for detection—an “active timescale” of 10 5 −10 6 yr, requiring observation while the object remains sufficiently young. Our results suggest that LISA could detect a few dozen highly magnetized WDs across the Galaxy during its mission. As a specific case, we investigate ZTF J1901+1458—a compact, massive, fast-rotating, and strongly magnetized WD with spin period ∼416 s and inferred surface field ∼10 9 G. We find that this object would be detectable by LISA with 4 yr of continuous data. This highlights the potential of CGW observations to probe magnetic field structure in WDs and their role in Type Ia supernova progenitors.

We introduce a novel high-resolution cluster simulation designed to serve as the massive halo counterpart of the modern cosmological galaxy evolution framework. The zoom-in simulation targets a volume of 4.1σ overdensity region, which is expected to evolve into a galaxy cluster with a virial mass of 5 M_⊙, comparable to that of the Virgo Cluster. The zoom-in volume extends out to 3.5 virial radii from the central halo. The novelties of M_⊙ is effective for tracing the early assembly of massive galaxies as well as the formation of dwarf galaxies. The spatial resolution of 68,parsecs in the best-resolved regions in the adaptive-mesh-refinement approach is a powerful tool for studying the detailed kinematic structure of galaxies. The time interval between snapshots is also exceptionally short (i.e., 15 Myr). This is ideal for monitoring changes in the physical properties of galaxies, particularly during their orbital motion within a larger halo. The simulation includes up-to-date feedback schemes for supernovae (SNe) and active galactic nuclei (AGNs). The chemical evolution is calculated for ten elements, along with dust calculation that includes the formation, size change, and destruction. To overcome the limitations of the Eulerian approach used for gas dynamics in this study, we employed Monte Carlo-based tracer particles in 10^ 14 are exemplified by its resolution. Its stellar mass resolution of 2 10^ 4 enabling a wide range of scientific investigations. The simulation has passed z=0.8, covering well over half of its cosmic history. We released the early data with the expectation they will facilitate studies of the early evolution of galaxies and overdensities.

Abstract We present 3D hydrodynamical modelling of supernova (SN)-induced binary-interaction-powered SNe; a scenario proposed for the peculiar type Ic SN SN2022jli. In this scenario, SN ejecta of a stripped-envelope star impact a close-by stellar companion, temporarily inflating the envelope. The expanded envelope engulfs the neutron star (NS), causing strong mass accretion at super-Eddington rates. Feedback from the accretion powers the SN light curve with periodic undulations. Our simulations capture key features of SN2022jli, both the overall decline and the superimposed undulations of the light curve. Based on our parameter study, we find that (i) the accretion feedback should be sufficiently geometrically confined and (ii) the eccentricity of the post-SN binary orbit should be 0.8 ≲ e ≲ 0.9 to sustain a high accretion rate and match the low undulation amplitude (Δ L / L ∼ 0.1) of SN2022jli. Different combinations of parameters could account for other SNe like SN2022mop, SN2009ip and SN2015ap, which have varying undulation periods and amplitudes. We also discuss possible explanations for other key features of SN2022jli such as the γ -ray detection at ∼200 days and the rapid optical drop at ∼250 days. Finally, we speculate on the future evolution of the system and its relation to existing NS binaries.