RAS_WEB (Page 2,435)

Redshifted 21-cm bispectrum II: Impact of the spin temperature fluctuations and redshift space distortions on the signal from the Cosmic Dawn. (arXiv:2012.11616v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Kamran_M/0/1/0/all/0/1">Mohd Kamran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ghara_R/0/1/0/all/0/1">Raghunath Ghara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Majumdar_S/0/1/0/all/0/1">Suman Majumdar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mondal_R/0/1/0/all/0/1">Rajesh Mondal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mellema_G/0/1/0/all/0/1">Garrelt Mellema</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bharadwaj_S/0/1/0/all/0/1">Somnath Bharadwaj</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pritchard_J/0/1/0/all/0/1">Jonathan R. Pritchard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Iliev_I/0/1/0/all/0/1">Ilian T. Iliev</a> We present a study of the 21-cm signal bispectrum (which quantifies the non-Gaussianity in the signal) from the Cosmic Dawn (CD). For our analysis, we have simulated the 21-cm signal using radiative transfer code GRIZZLY, while considering two types of sources (mini-QSOs and HMXBs) for Ly$alpha$ coupling and the X-ray heating of the IGM. UsingRead More →

Intermediate-mass Black Holes from High Massive-star Binary Fractions in Young Star Clusters. (arXiv:2012.10497v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Gonzalez_E/0/1/0/all/0/1">Elena Gonz&#xe1;lez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kremer_K/0/1/0/all/0/1">Kyle Kremer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chatterjee_S/0/1/0/all/0/1">Sourav Chatterjee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fragione_G/0/1/0/all/0/1">Giacomo Fragione</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_C/0/1/0/all/0/1">Carl L. Rodriguez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weatherford_N/0/1/0/all/0/1">Newlin C. Weatherford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ye_C/0/1/0/all/0/1">Claire S. Ye</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rasio_F/0/1/0/all/0/1">Frederic A. Rasio</a> Black holes formed in dense star clusters, where dynamical interactions are frequent, may have fundamentally different properties than those formed through isolated stellar evolution. Theoretical models for single star evolution predict a gap in the black hole mass spectrum from roughly $40-120,M_{odot}$ caused by (pulsational) pair-instability supernovae. Motivated by the recent LIGO/Virgo event GW190521, we investigate whether black holes with masses withinRead More →

Improved near optimal angular quadratures for polarised radiative transfer in 3D MHD models. (arXiv:2012.04981v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Bestard_J/0/1/0/all/0/1">Jaume Jaume Bestard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stepan_J/0/1/0/all/0/1">Ji&#x159;&#xed; &#x160;t&#x11b;p&#xe1;n</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bueno_J/0/1/0/all/0/1">Javier Trujillo Bueno</a> Accurate angular quadratures are crucial for the numerical solution of three-dimensional (3D) radiative transfer problems, especially when the spectral line polarisation produced by the scattering of anisotropic radiation is included. There are two requirements for obtaining an optimal quadrature and they are difficult to satisfy simultaneously: high accuracy and short computing time. By imposing certain symmetries, we were recently able to derive a set of near optimal angular quadratures. Here, we extend our previous investigation by considering otherRead More →

Distinguishing AGN from starbursts as the origin of double peaked Lyman-Alpha Emitters in the reionization era. (arXiv:2012.00014v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Padmanabhan_H/0/1/0/all/0/1">Hamsa Padmanabhan</a> (Geneva), <a href="http://arxiv.org/find/astro-ph/1/au:+Loeb_A/0/1/0/all/0/1">Abraham Loeb</a> (Harvard) We discuss the possible origin of the double-peaked profiles recently observed in Lyman-Alpha Emitters (LAEs) at the epoch of reionization ($z gtrsim 6.5$) from obscured active galactic nuclei (AGN). Combining the extent of the Lyman-$alpha$ near-zones estimated from the blue peak velocity offset in these galaxies, with the ionizing emissivity of quasars at $z gtrsim 6$, we forecast the intrinsic UV and X-ray luminosities of the AGN needed to give rise to their double-peaked profiles. We also estimateRead More →

2HDM singlet portal to dark matter. (arXiv:2011.09101v2 [hep-ph] UPDATED) <a href="http://arxiv.org/find/hep-ph/1/au:+Cabrera_M/0/1/0/all/0/1">M. E. Cabrera</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Casas_J/0/1/0/all/0/1">J. A. Casas</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Delgado_A/0/1/0/all/0/1">A. Delgado</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Robles_S/0/1/0/all/0/1">S. Robles</a> Higgs portal models are the most minimal way to explain the relic abundance of the Universe. They add just a singlet that only couples to the Higgs through a single parameter that controls both the dark matter relic abundance and the direct detection cross-section. Unfortunately this scenario, either with scalar or fermionic dark matter, is almost ruled out by the latter. In this paper we analyze the Higgs-portal idea with fermionic dark matter in the context of a 2HDM. By disentangling theRead More →

Higgsino Dark Matter in the MSSM. (arXiv:2008.00954v2 [hep-ph] UPDATED) <a href="http://arxiv.org/find/hep-ph/1/au:+Delgado_A/0/1/0/all/0/1">Antonio Delgado</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Quiros_M/0/1/0/all/0/1">Mariano Quir&#xf3;s</a> A comologically stable neutral component from a nearly pure $SU(2)$ doublet, with a mass $sim$1.1 TeV, is one appealing candidate for dark matter (DM) consistent with all direct dark matter searches. We have explored this possibility in the context of the Minimal Supersymmetric extension of the Standard Model (MSSM), with the Higgsino playing the role of DM, in theories where supersymmetry breaking is transmitted by gravitational interactions at the unification scale $Msimeq 2times 10^{16}$ GeV. We have focussed our work in the search of “light” supersymmetric spectra, which could beRead More →

Properties of polarized synchrotron emission from fluctuation-dynamo action — I. Application to galaxy clusters. (arXiv:2011.08499v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Sur_S/0/1/0/all/0/1">Sharanya Sur</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Basu_A/0/1/0/all/0/1">Aritra Basu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Subramanian_K/0/1/0/all/0/1">Kandaswamy Subramanian</a> Using magnetohydrodynamic simulations of fluctuation dynamos, we perform broad-bandwidth synthetic observations to investigate the properties of polarized synchrotron emission and the role that Faraday rotation plays in inferring the polarized structures in the intracluster medium (ICM) of galaxy clusters. In the saturated state of the dynamo, we find a Faraday depth (FD) dispersion $sigma_{rm FD} approx 100$ rad m$^{-2}$, in agreement with observed values in the ICM. Remarkably, the FD power spectrum is qualitatively similar to $M(k)/k$, where $M(k)$Read More →

Late-time Observations of Calcium-Rich Transient SN 2019ehk Reveal a Pure Radioactive Decay Power Source. (arXiv:2010.15863v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Jacobson_Galan_W/0/1/0/all/0/1">Wynn V. Jacobson-Gal&#xe1;n</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Margutti_R/0/1/0/all/0/1">Raffaella Margutti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kilpatrick_C/0/1/0/all/0/1">Charles D. Kilpatrick</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Raymond_J/0/1/0/all/0/1">John Raymond</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berger_E/0/1/0/all/0/1">Edo Berger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blanchard_P/0/1/0/all/0/1">Peter K. Blanchard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bobrick_A/0/1/0/all/0/1">Alexey Bobrick</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Foley_R/0/1/0/all/0/1">Ryan J. Foley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gomez_S/0/1/0/all/0/1">Sebastian Gomez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hosseinzadeh_G/0/1/0/all/0/1">Griffin Hosseinzadeh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Milisavljevic_D/0/1/0/all/0/1">Danny Milisavljevic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perets_H/0/1/0/all/0/1">Hagai Perets</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Terreran_G/0/1/0/all/0/1">Giacomo Terreran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zenati_Y/0/1/0/all/0/1">Yossef Zenati</a> We present $textit{Hubble Space Telescope}$ imaging of the Calcium-rich supernova (SN) 2019ehk at 276 – 389 days after explosion. These observations represent the latest photometric measurements of a Calcium-rich transient to date and allows for the first opportunity to analyze the late-timeRead More →

Large-scale variation in reionization history caused by Baryon-dark matter streaming velocity. (arXiv:2010.12374v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Park_H/0/1/0/all/0/1">Hyunbae Park</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shapiro_P/0/1/0/all/0/1">Paul R. Shapiro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ahn_K/0/1/0/all/0/1">Kyungjin Ahn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yoshida_N/0/1/0/all/0/1">Naoki Yoshida</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hirano_S/0/1/0/all/0/1">Shingo Hirano</a> At cosmic recombination, there was supersonic relative motion between baryons and dark matter, which originated from the baryonic acoustic oscillations in the early universe. This motion has been considered to have a negligible impact on the late stage of cosmic reionization because the relative velocity quickly decreases. However, recent studies have suggested that the recombination in gas clouds smaller than the local Jeans mass ($lesssim$ $10^8~M_odot$) can affect the reionization history by boosting the numberRead More →

Tidal Dissipation in Dual-Body, Highly Eccentric, and Non-synchronously Rotating Systems: Applications to Pluto-Charon and the Exoplanet TRAPPIST-1e. (arXiv:2010.11801v2 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Renaud_J/0/1/0/all/0/1">Joe P. Renaud</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Henning_W/0/1/0/all/0/1">Wade G. Henning</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Saxena_P/0/1/0/all/0/1">Prabal Saxena</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Neveu_M/0/1/0/all/0/1">Marc Neveu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bagheri_A/0/1/0/all/0/1">Amirhossein Bagheri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mandell_A/0/1/0/all/0/1">Avi Mandell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hurford_T/0/1/0/all/0/1">Terry Hurford</a> Using the Andrade-derived Sundberg-Cooper rheology, we apply several improvements to the secular tidal evolution of TRAPPIST-1e and the early history of Pluto-Charon under the simplifying assumption of homogeneous bodies. By including higher-order eccentricity terms (up to and including $e^{20}$), we find divergences from the traditionally used $e^{2}$ truncation starting around $e=0.1$. Order-of-magnitude differences begin to occur for $e>0.6$. Critically, higher-order eccentricity termsRead More →

Annihilating Dark Matter Search with 12 Years of Fermi LAT Data in Nearby Galaxy Clusters. (arXiv:2010.11006v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Thorpe_Morgan_C/0/1/0/all/0/1">Charles Thorpe-Morgan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Malyshev_D/0/1/0/all/0/1">Denys Malyshev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stegen_C/0/1/0/all/0/1">Christoph-Alexander Stegen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Santangelo_A/0/1/0/all/0/1">Andrea Santangelo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jochum_J/0/1/0/all/0/1">Josef Jochum</a> Galaxy clusters are the largest virialised objects in the Universe, and as such, have a high dark matter (DM) concentration. This abundance of dark matter makes them promising targets for indirect DM searches. Here we report the details of a search, utilising almost 12~years of Fermi/LAT data, for gamma ray signatures from the pair annihilation of WIMP dark matter in the GeV energy band. From this, we present the constraints on theRead More →

Testing the star formation scaling relations in the clumps of the North American and Pelican cloud complexes. (arXiv:2010.07333v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Das_S/0/1/0/all/0/1">Swagat R. Das</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jose_J/0/1/0/all/0/1">Jessy Jose</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Samal_M/0/1/0/all/0/1">Manash R Samal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_S/0/1/0/all/0/1">Shaobo Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Panwar_N/0/1/0/all/0/1">Neelam Panwar</a> The processes which regulate the star-formation within molecular clouds are still not well understood. Various star-formation scaling relations have been proposed to explain this issue by formulating a relation between star-formation rate surface density ($rm Sigma_{SFR}$) and the underlying gas surface density ($rm Sigma_{gas}$). In this work, we test various star formation scaling relations, such as Kennicutt-Schmidt relation, volumetric star-formation relation, orbital time model, crossing time model, andRead More →

The infrared-radio correlation of star-forming galaxies is strongly M$_{star}$-dependent but nearly redshift-invariant since z$sim$4. (arXiv:2010.05510v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Delvecchio_I/0/1/0/all/0/1">I. Delvecchio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Daddi_E/0/1/0/all/0/1">E. Daddi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sargent_M/0/1/0/all/0/1">M. T. Sargent</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jarvis_M/0/1/0/all/0/1">M. J. Jarvis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Elbaz_D/0/1/0/all/0/1">D. Elbaz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jin_S/0/1/0/all/0/1">S. Jin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_D/0/1/0/all/0/1">D. Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Whittam_I/0/1/0/all/0/1">I. H. Whittam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Algera_H/0/1/0/all/0/1">H. Algera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carraro_R/0/1/0/all/0/1">R. Carraro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DEugenio_C/0/1/0/all/0/1">C. D&#x27;Eugenio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Delhaize_J/0/1/0/all/0/1">J. Delhaize</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kalita_B/0/1/0/all/0/1">B. S. Kalita</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leslie_S/0/1/0/all/0/1">S. Leslie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Molnar_D/0/1/0/all/0/1">D. Cs. Molnar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Novak_M/0/1/0/all/0/1">M. Novak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prandoni_I/0/1/0/all/0/1">I. Prandoni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smolcic_V/0/1/0/all/0/1">V. Smolcic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ao_Y/0/1/0/all/0/1">Y. Ao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aravena_M/0/1/0/all/0/1">M. Aravena</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bournaud_F/0/1/0/all/0/1">F. Bournaud</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Collier_J/0/1/0/all/0/1">J. D. Collier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Randriamampandry_S/0/1/0/all/0/1">S. M. Randriamampandry</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Randriamanakoto_Z/0/1/0/all/0/1">Z. Randriamanakoto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodighiero_G/0/1/0/all/0/1">G. Rodighiero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schober_J/0/1/0/all/0/1">J. Schober</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+White_S/0/1/0/all/0/1">S. V.Read More →

Primordial black holes from long-range scalar forces and scalar radiative cooling. (arXiv:2008.12456v3 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Flores_M/0/1/0/all/0/1">Marcos M. Flores</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kusenko_A/0/1/0/all/0/1">Alexander Kusenko</a> We describe a new scenario for the formation of primordial black holes (PBHs). In the early Universe, the long-range forces mediated by the scalar fields can lead to formation of halos of heavy particles even during the radiation-dominated era. The same interactions result in the emission of scalar radiation from the motion and close encounters of particles in such halos. Radiative cooling due the scalar radiation allows the halos to collapse to black holes. We illustrate this scenario on a simple model with fermionsRead More →

Evolving traversable wormholes satisfying the energy conditions in the presence of pole dark energy. (arXiv:2008.04013v3 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Zangeneh_M/0/1/0/all/0/1">Mahdi Kord Zangeneh</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Lobo_F/0/1/0/all/0/1">Francisco S. N. Lobo</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Moradpour_H/0/1/0/all/0/1">Hooman Moradpour</a> We consider the evolution of traversable wormhole geometries in the inflationary, radiation — and matter — dominated eras, and dynamic wormholes with a traceless energy-momentum tensor (EMT), within the recently proposed {it pole dark energy} model. We show that the evolving radiation — and matter — dominated wormhole spacetimes satisfy the null energy condition (NEC), but possess negative energy densities at late times, thus violating the weak energy condition (WEC) in this specific domain. However, weRead More →

Nigraha: Machine-learning based pipeline to identify and evaluate planet candidates from TESS. (arXiv:2101.09227v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Rao_S/0/1/0/all/0/1">Sriram Rao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mahabal_A/0/1/0/all/0/1">Ashish Mahabal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rao_N/0/1/0/all/0/1">Niyanth Rao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Raghavendra_C/0/1/0/all/0/1">Cauligi Raghavendra</a> The Transiting Exoplanet Survey Satellite (TESS) has now been operational for a little over two years, covering the Northern and the Southern hemispheres once. The TESS team processes the downlinked data using the Science Processing Operations Center pipeline and Quick Look pipeline to generate alerts for follow-up. Combined with other efforts from the community, over two thousand planet candidates have been found of which tens have been confirmed as planets. We present our pipeline, Nigraha, that is complementary toRead More →

On the radial structure of planetary bodies formed by the streaming instability. (arXiv:2101.09209v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Visser_R/0/1/0/all/0/1">Rico G. Visser</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Drazkowska_J/0/1/0/all/0/1">Joanna Dr&#x105;&#x17c;kowska</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dominik_C/0/1/0/all/0/1">Carsten Dominik</a> Comets and small planetesimals are believed to contain primordial building blocks in the form of millimeter to centimeter sized pebbles. One of the viable growing mechanisms to form these small bodies is through the streaming instability (SI) in which pebbles cluster and gravitationally collapse towards a planetesimal or comet in the presence of gas drag. However, most SI simulations are global and lack the resolution to follow the final collapse stage of a pebble cloud within its Hill radius. We aimRead More →

Quantifying uncertainties in the solar axion flux and their impact on determining axion model parameters. (arXiv:2101.08789v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Hoof_S/0/1/0/all/0/1">Sebastian Hoof</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Jaeckel_J/0/1/0/all/0/1">Joerg Jaeckel</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Thormaehlen_L/0/1/0/all/0/1">Lennert J. Thormaehlen</a> We review the calculation of the solar axion flux from axion-photon and axion-electron interactions and survey the available solar models and opacity codes. We develop a publicly available C++/Python code to quantify the associated systematic differences and statistical fluctuations. The number of axions emitted in helioseismological solar models is systematically larger by about 5% compared to photospheric models, while the overall statistical uncertainties in solar models are typically at the percent level in both helioseismological and photospheric models.Read More →

Testing the role of environmental effects on the Initial Mass Function of low mass stars. (arXiv:2101.08804v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Damian_B/0/1/0/all/0/1">Belinda Damian</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Jose_J/0/1/0/all/0/1">Jessy Jose</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Samal_M/0/1/0/all/0/1">Manash R. Samal</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Moraux_E/0/1/0/all/0/1">Estelle Moraux</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Das_S/0/1/0/all/0/1">Swagat R. Das</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Patra_S/0/1/0/all/0/1">Sudeshna Patra</a> (1) ((1) IISER Tirupati, India, (2) PRL, India, (3) Univ. Grenoble Alpes, France) In star formation process, the vital role of environmental factors such as feedback from massive stars and stellar density on the form of the Initial Mass Function (IMF) at low-mass end is yet to be understood. Hence a systematic, high sensitive observational analysis of a sample of regions under diverseRead More →

Reheating in small-field inflation on the brane: The Swampland Criteria and observational constraints in light of the PLANCK 2018 results. (arXiv:2101.08882v1 [hep-th]) <a href="http://arxiv.org/find/hep-th/1/au:+Osses_C/0/1/0/all/0/1">Constanza Osses</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Videla_N/0/1/0/all/0/1">Nelson Videla</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Panotopoulos_G/0/1/0/all/0/1">Grigoris Panotopoulos</a> We study cosmological inflation and its dynamics in the framework of the Randall-Sundrum II brane model. In particular, we analyze in detail four representative small-field inflationary potentials, namely Natural inflation, Hilltop inflation, Higgs-like inflation, and Exponential SUSY inflation, each characterized by two mass scales. We constrain the parameters for which a viable inflationary Universe emerges using the latest PLANCK results. Furthermore, we investigate whether or not those models in brane cosmology are consistent withRead More →