Probing the surface environment of large T-type asteroids. (arXiv:2206.11672v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kwon_Y/0/1/0/all/0/1">Yuna G. Kwon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hasegawa_S/0/1/0/all/0/1">Sunao Hasegawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fornasier_S/0/1/0/all/0/1">Sonia Fornasier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ishiguro_M/0/1/0/all/0/1">Masateru Ishiguro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Agarwal_J/0/1/0/all/0/1">Jessica Agarwal</a> We probed the surface environment of large ($>$80 km in diameter) T-type asteroids, a taxonomic type relatively ill-constrained as an independent group, and discussed their place of origin. We performed spectroscopic observations of two T-type asteroids, (96) Aegle and (570) Kythera, over 2.8–4.0 $mu$m using the Subaru telescope. With other T-types’ spectra available in the literature and survey datasets, we strove to find commonalities and global trends in this group. We also utilised the asteroids’ polarimetric data and meteoriteRead More →

Inverse energy cascade in self-gravitating collisionless dark matter flow and effects of halo shape. (arXiv:2110.13885v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Zhijie/0/1/0/all/0/1">Zhijie</a> (Jay)Xu Halo-mediated mass and energy cascades are key to understand dark matter flow. Both cascades origin from the mass exchange between halo and out-of-halo sub-systems. Kinetic energy can be from the motion of halos and particle motion in halos. Similarly, potential energy can be due to the inter- and intra-halo interactions. Intra-halo virial equilibrium is established much faster than inter-halo. Change of energy of entire system comes from virilization in halos. At statistically steady state, continuous mass exchange is required to sustain growth of total haloRead More →

X-ray polarimetry-timing. (arXiv:2206.11671v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Ingram_A/0/1/0/all/0/1">Adam Ingram</a> X-ray polarimetry-timing is the characterization of rapid variability in the X-ray polarization degree and angle. As for the case of spectral-timing, it provides causal information valuable for reconstructing indirect maps of the vicinity of compact objects. To call X-ray polarimetry-timing a young field is somewhat of an understatement, given that the first X-ray mission truly capable of enabling polarimetry-timing analyses has only just launched at the time of writing. Now is therefore an exciting time for the field, in which we have theoretical predictions and are eagerly awaiting data. This Chapter discusses the theoretical expectations and also describesRead More →

Cosmic-ray electron transport in the galaxy M 51. (arXiv:2206.11670v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Dorner_J/0/1/0/all/0/1">Julien D&#xf6;rner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reichherzer_P/0/1/0/all/0/1">Patick Reichherzer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tjus_J/0/1/0/all/0/1">Julia Becker Tjus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heesen_V/0/1/0/all/0/1">Volker Heesen</a> Indirect observations of the cosmic-ray electron (CRE) distribution via synchrotron emission is crucial for deepening the understanding of the CRE transport in the interstellar medium, and in investigating the role of galactic outflows. In this paper, we quantify the contribution of diffusion and advection dominated transport of cosmic-ray electrons in the galaxy M51 considering relevant energy loss processes. We use recent measurement from M51 that allow for the derivation of the diffusion coefficient, the star formation rate, and the magnetic field strength.Read More →

Modelling the transport of relativistic solar protons along a heliospheric current sheet during historic GLE events. (arXiv:2206.11650v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Waterfall_C/0/1/0/all/0/1">Charlotte O. G. Waterfall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dalla_S/0/1/0/all/0/1">Silvia Dalla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Laitinen_T/0/1/0/all/0/1">Timo Laitinen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hutchinson_A/0/1/0/all/0/1">Adam Hutchinson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marsh_M/0/1/0/all/0/1">Mike Marsh</a> There are many difficulties associated with forecasting high-energy solar particle events at Earth. One issue is understanding why some large solar eruptive events trigger ground level enhancement (GLE) events and others do not. In this work we perform 3D test particle simulations of a set of historic GLEs to understand more about what causes these powerful events. Particular focus is given to studying how the heliospheric current sheet (HCS) affectsRead More →

V1294 Aql = HD 184279: A bad boy among Be stars or an important clue to the Be phenomenon?. (arXiv:2206.11649v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Harmanec_P/0/1/0/all/0/1">P. Harmanec</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bozic_H/0/1/0/all/0/1">H. Bo&#x17e;i&#x107;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koubsky_P/0/1/0/all/0/1">P. Koubsk&#xfd;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_S/0/1/0/all/0/1">S. Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ruzdjak_D/0/1/0/all/0/1">D. Ru&#x17e;djak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sudar_D/0/1/0/all/0/1">D. Sudar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Slechta_M/0/1/0/all/0/1">M. &#x160;lechta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wolf_M/0/1/0/all/0/1">M. Wolf</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Korcakova_D/0/1/0/all/0/1">D. Kor&#x10d;&#xe1;kov&#xe1;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zasche_P/0/1/0/all/0/1">P. Zasche</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oplistilova_A/0/1/0/all/0/1">A. Opli&#x161;tilov&#xe1;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vrsnak_D/0/1/0/all/0/1">D. Vr&#x161;nak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ak_H/0/1/0/all/0/1">H. Ak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eenens_P/0/1/0/all/0/1">P. Eenens</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bakis_H/0/1/0/all/0/1">H. Baki&#x15f;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bakis_V/0/1/0/all/0/1">V. Baki&#x15f;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Otero_S/0/1/0/all/0/1">S. Otero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chini_R/0/1/0/all/0/1">R. Chini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Demsky_T/0/1/0/all/0/1">T. Demsky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barlow_B/0/1/0/all/0/1">B.N. Barlow</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Svoboda_P/0/1/0/all/0/1">P. Svoboda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jonak_J/0/1/0/all/0/1">J. Jon&#xe1;k</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vitovsky_K/0/1/0/all/0/1">K. Vitovsk&#xfd;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harmanec_A/0/1/0/all/0/1">A. Harmanec</a> A reliable determination of the basic physical properties and variability patterns ofRead More →

Improved binary solution for the gamma-ray binary 1FGL J1018.6-5856. (arXiv:2206.11647v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Soelen_B/0/1/0/all/0/1">B. van Soelen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Keague_S/0/1/0/all/0/1">S. Mc Keague</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Malyshev_D/0/1/0/all/0/1">D. Malyshev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chernyakova_M/0/1/0/all/0/1">M. Chernyakova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Komin_N/0/1/0/all/0/1">N. Komin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matchett_N/0/1/0/all/0/1">N. Matchett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Monageng_I/0/1/0/all/0/1">I.M. Monageng</a> The gamma-ray binary 1FGL J1018.6-5856 consists of an O6V((f)) type star and an unknown compact object, and shows orbitally modulated emission from radio to very high energy gamma rays. The X-ray light curve shows a maximum around the same phase as the GeV emission, but also a secondary maximum between phases $phi=0.2 – 0.6$. A clear solution to the binary system is important for understanding the emission mechanisms occurring within theRead More →

The Nature of Luminous Quasars with Very Large C IV Equivalent Widths. (arXiv:2206.11631v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Fu_S/0/1/0/all/0/1">Shuqi Fu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brandt_W/0/1/0/all/0/1">W. N. Brandt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zou_F/0/1/0/all/0/1">Fan Zou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Laor_A/0/1/0/all/0/1">Ari Laor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garmire_G/0/1/0/all/0/1">Gordon P. Garmire</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ni_Q/0/1/0/all/0/1">Qingling Ni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Timlin_J/0/1/0/all/0/1">John D. Timlin III</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xue_Y/0/1/0/all/0/1">Yongquan Xue</a> We report results for a complete sample of ten luminous radio-quiet quasars with large C IV equivalent widths (EW > 150 A). For 8/10 we performed Chandra snapshot observations. We find that, in addition to the enhanced C IV line EW, their He II and Mg II lines are enhanced, but the C III] line is not. Their X-ray emission is substantially strongerRead More →

Laboratory Experiments on the Radiation Astrochemistry of Water Ice Phases. (arXiv:2206.11614v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Mifsud_D/0/1/0/all/0/1">Duncan V. Mifsud</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hailey_P/0/1/0/all/0/1">Perry A. Hailey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Herczku_P/0/1/0/all/0/1">P&#xe9;ter Herczku</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Juhasz_Z/0/1/0/all/0/1">Zolt&#xe1;n Juh&#xe1;sz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kovacs_S/0/1/0/all/0/1">S&#xe1;ndor T. S. Kov&#xe1;cs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sulik_B/0/1/0/all/0/1">B&#xe9;la Sulik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ioppolo_S/0/1/0/all/0/1">Sergio Ioppolo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kanuchova_Z/0/1/0/all/0/1">Zuzana Ka&#x148;uchov&#xe1;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McCullough_R/0/1/0/all/0/1">Robert W. McCullough</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Paripas_B/0/1/0/all/0/1">B&#xe9;la Parip&#xe1;s</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mason_N/0/1/0/all/0/1">Nigel J. Mason</a> Water (H2O) ice is ubiquitous component of the universe, having been detected in a variety of interstellar and Solar System environments where radiation plays an important role in its physico-chemical transformations. Although the radiation chemistry of H2O astrophysical ice analogues has been well studied, direct and systematic comparisons of different solid phases are scarceRead More →

Starspots Modelling and Flare Analysis on Selected MV Stars. (arXiv:2206.11611v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Bicz_K/0/1/0/all/0/1">Kamil Bicz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Falewicz_R/0/1/0/all/0/1">Robert Falewicz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pietras_M/0/1/0/all/0/1">Ma&#x142;gorzata Pietras</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Siarkowski_M/0/1/0/all/0/1">Marek Siarkowski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pres_P/0/1/0/all/0/1">Pawe&#x142; Pre&#x15b;</a> We studied light curves of GJ 1243, YZ CMi, and V374 Peg, observed by TESS for the presence of stellar spots and stellar flares. One of the main goals was to model light curves of spotted stars to estimate the number of spots along with their parameters using our original BASSMAN software. The modeled light curves were subtracted from the observations to increase efficiency of flare detection. Flares were detected automatically with our new dedicated software WARPFINDER. We estimatedRead More →

VISH$nu$: a unified solution to five SM shortcomings with a protected electroweak scale. (arXiv:2206.11598v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Sopov_A/0/1/0/all/0/1">Alexei H. Sopov</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Volkas_R/0/1/0/all/0/1">Raymond R. Volkas</a> We propose a Standard Model extension, coined VISH$nu$ (Variant-axIon Seesaw Higgs $nu$-trino), that is a variation of its predecessor, the $nu$DFSZ model. In accounting for the origin of neutrino masses, dark matter and the baryon asymmetry of the universe, VISH$nu$ inherits the explanatory power of $nu$DFSZ while, of course, resolving the strong $CP$ problem. In both models, the electroweak scale is naturally protected in the presence of a high seesaw scale that is identified with the Peccei-Quinn (PQ) spontaneous symmetry breaking scale.Read More →

Gap opening by planets in discs with magnetised winds. (arXiv:2206.11595v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Elbakyan_V/0/1/0/all/0/1">Vardan Elbakyan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wu_Y/0/1/0/all/0/1">Yinhao Wu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nayakshin_S/0/1/0/all/0/1">Sergei Nayakshin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosotti_G/0/1/0/all/0/1">Giovanni Rosotti</a> Planets open deep gaps in protoplanetary discs when their mass exceeds a gap opening mass, $M_{rm gap}$. We use one- and two-dimensional simulations to study planet gap opening in discs with angular momentum transport powered by MHD disc winds. We parameterise the efficiency of the MHD disc wind angular momentum transport through a dimensionless parameter $alpha_{rm dw}$, which is an analogue to the turbulent viscosity $alpha_{rm v}$. We find that magnetised winds are much less efficient in counteracting planet tidal torques thanRead More →

Cosmological evolution in Weyl conformal geometry. (arXiv:2110.07056v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Ghilencea_D/0/1/0/all/0/1">D. M. Ghilencea</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Harko_T/0/1/0/all/0/1">T. Harko</a> We discuss the cosmological evolution of the Weyl conformal geometry and its associated Weyl quadratic gravity. The Einstein gravity (with a positive cosmological constant) is recovered in the spontaneously broken phase of Weyl gravity; this happens after the Weyl gauge field ($omega_mu$) of scale symmetry, that is part of the Weyl geometry, becomes massive by Stueckelberg mechanism and then decouples. This breaking is a natural result of the cosmological evolution of Weyl geometry, in the absence of matter. Of particular interest in the analysis is the special limiting caseRead More →

Polarized Vector Oscillons. (arXiv:2111.08700v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_H/0/1/0/all/0/1">Hong-Yi Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jain_M/0/1/0/all/0/1">Mudit Jain</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amin_M/0/1/0/all/0/1">Mustafa A. Amin</a> Oscillons are spatially localized, time-periodic and long-lived configurations that were primarily proposed in scalar field theories with attractive self-interactions. In this letter, we demonstrate that oscillons also exist in the low-energy effective theory of an interacting massive (real) vector field. We provide two types of vector oscillons with vanishing orbital angular momentum, and approximately spherically symmetric energy density, but not field configurations. These are: (1) “directional” oscillons (linearly polarized), with vanishing total intrinsic spin, and (2) “spinning” oscillons (circularly polarized) with a macroscopic instrinsic spin equal to $hbartimes$ numberRead More →

CONCERTO : Digital processing for finding and tuning LEKIDs. (arXiv:2206.11554v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Bounmy_J/0/1/0/all/0/1">Julien Bounmy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hoarau_C/0/1/0/all/0/1">Christophe Hoarau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Macias_Perez_J/0/1/0/all/0/1">Juan-Francisco Mac&#xed;as-P&#xe9;rez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beelen_A/0/1/0/all/0/1">Alexandre Beelen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benoit_A/0/1/0/all/0/1">Alain Beno&#xee;t</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bourrion_O/0/1/0/all/0/1">Olivier Bourrion</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calvo_M/0/1/0/all/0/1">Martino Calvo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Catalano_A/0/1/0/all/0/1">Andrea Catalano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fasano_A/0/1/0/all/0/1">Alessandro Fasano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Goupy_J/0/1/0/all/0/1">Johannes Goupy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lagache_G/0/1/0/all/0/1">Guilaine Lagache</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marpaud_J/0/1/0/all/0/1">Julien Marpaud</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Monfardini_A/0/1/0/all/0/1">Alessandro Monfardini</a> We describe the on-line algorithms developed to probe Lumped Element Kinetic Inductance Detectors (LEKID) in this paper. LEKIDs are millimeter wavelength detectors for astronomy. LEKID arrays are currently operated in different instruments as: NIKA2 at the IRAM telescope in Spain, KISS at the Teide Observatory telescope in Tenerife, and CONCERTO at the APEX 12-meter telescopeRead More →

Molecular gas dynamics around nuclei of galaxies. (arXiv:2205.06106v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Combes_F/0/1/0/all/0/1">Francoise Combes</a> (Obs-Paris, LERMA) Recent molecular line observations with ALMA in several nearby Seyferts have revealed the existence of molecular tori, and the nature of gas flows at 10-20~pc scale. At 100~pc scale, or kpc-scale, previous NOEMA work on gravitational torques had shown that only about one third of Seyfert galaxies experienced molecular inflow and central fueling, while in most cases the gas was stalled in rings. At higher resolution, i.e. 10-20~pc scale, it is possible now to see in some cases AGN fueling due to nuclear trailing spirals, influenced by the black holeRead More →

Moving Groups Across Galactocentric Radius with Gaia DR3. (arXiv:2206.10633v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Lucchini_S/0/1/0/all/0/1">Scott Lucchini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pellett_E/0/1/0/all/0/1">Emil Pellett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DOnghia_E/0/1/0/all/0/1">Elena D&#x27;Onghia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aguerri_J/0/1/0/all/0/1">J. Alfonso L. Aguerri</a> The kinematic plane of stars near the Sun has proven an indispensable tool for untangling the complexities of the structure of our Milky Way (MW). With ever improving data, numerous kinematic “moving groups” of stars have been better characterized and new ones continue to be discovered. Here we present an improved method for detecting these groups using MGwave, a new open-source 2D wavelet transformation code that we have developed. Our code implements similar techniques to previous wavelet software; however, weRead More →

Could the “Wow” signal have originated from a stochastic repeating beacon?. (arXiv:2206.08374v2 [astro-ph.IM] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Kipping_D/0/1/0/all/0/1">David Kipping</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gray_R/0/1/0/all/0/1">Robert Gray</a> The famous “Wow” signal detected in 1977 remains arguably the most compelling SETI signal ever found. The original Big Ear data requires that the signal turned on/off over the span of ~3 minutes (time difference between the dual antennae), yet persisted for 72 seconds (duration of a single beam sweep). Combined with the substantial and negative follow-up efforts, these observations limit the allowed range of signal repeat schedules, to the extent that one might question the credibility of the signal itself. Previous work has largelyRead More →

Primordial Black Holes and Gravitational Waves in Multi-Axion-Chern-Simons Inflation. (arXiv:2206.07963v2 [hep-th] UPDATED) <a href="http://arxiv.org/find/hep-th/1/au:+Mavromatos_N/0/1/0/all/0/1">Nick E. Mavromatos</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Spanos_V/0/1/0/all/0/1">Vassilis C. Spanos</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Stamou_I/0/1/0/all/0/1">Ioanna D. Stamou</a> We study aspects of inflation and the possibility of enhanced production of primordial black holes (PBHs) and gravitational waves (GWs) in a string-inspired model of two axion fields coupled to Chern-Simons gravity, which results in a running-vacuum-model inflation. Fluctuations of the scale invariant spectrum, consistent with the cosmological data, are provided in this model by world-sheet (non-perturbative) instanton terms of the axion field arising from string compactification. As a result of such modulations, there is an enhanced production of PBHs andRead More →

The Equilibrium Tide: An Updated Prescription for Population Synthesis Codes. (arXiv:2206.06068v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Preece_H/0/1/0/all/0/1">Holly P. Preece</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hamers_A/0/1/0/all/0/1">Adrian S. Hamers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Neunteufel_P/0/1/0/all/0/1">Patrick G. Neunteufel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schafer_A/0/1/0/all/0/1">Adam L. Schafer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tout_C/0/1/0/all/0/1">Christopher A. Tout</a> We present an updated prescription for the equilibrium tides suitable for population synthesis codes. A grid of 1D evolutionary models was created and the viscous time-scale was calculated for each detailed model. A metallicity dependent power-law relation was fitted to both the convective cores and convective envelopes of the models. The prescription was implemented into the population synthesis code BSE and predicts an 16.5% reduction in the overall number of merges, withRead More →