An Extremely Energetic Supernova from a Very Massive Star in a Dense Medium
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Enhanced Mass Loss Rates in Red Supergiants and Their Impact in The
Revista Mexicana de Astronom´ıa y Astrof´ısica, 55, 161–175 (2019) DOI: https://doi.org/10.22201/ia.01851101p.2019.55.02.04 ENHANCED MASS LOSS RATES IN RED SUPERGIANTS AND THEIR IMPACT ON THE CIRCUMSTELLAR MEDIUM L. Hern´andez-Cervantes1,2, B. P´erez-Rend´on3, A. Santill´an4, G. Garc´ıa-Segura5, and C. Rodr´ıguez-Ibarra6 Received September 25 2018; accepted May 8 2019 ABSTRACT In this work, we present models of massive stars between 15 and 23 M⊙, with enhanced mass loss rates during the red supergiant phase. Our aim is to explore the impact of extreme red supergiant mass-loss on stellar evolution and on their cir- cumstellar medium. We computed a set of numerical experiments, on the evolution of single stars with initial masses of 15, 18, 20 and, 23 M⊙, and solar composi- tion (Z = 0.014), using the numerical stellar code BEC. From these evolutionary models, we obtained time-dependent stellar wind parameters, that were used ex- plicitly as inner boundary conditions in the hydrodynamical code ZEUS-3D, which simulates the gas dynamics in the circumstellar medium (CSM), thus coupling the stellar evolution to the dynamics of the CSM. We found that stars with extreme mass loss in the RSG phase behave as a larger mass stars. RESUMEN En este trabajo presentamos modelos evolutivos de estrellas en el intervalo de 15 a 23 M⊙, usando un incremento en la tasa de p´erdida de masa durante su fase de supergigante roja para explorar el impacto de una fuerte p´erdida de masa en la evoluci´on de la estrella y en la din´amica de su medio circunestelar. -
Correction: Corrigendum: the Superluminous Transient ASASSN
LETTERS PUBLISHED: 12 DECEMBER 2016 | VOLUME: 1 | ARTICLE NUMBER: 0002 The superluminous transient ASASSN-15lh as a tidal disruption event from a Kerr black hole G. Leloudas1,2*, M. Fraser3, N. C. Stone4, S. van Velzen5, P. G. Jonker6,7, I. Arcavi8,9, C. Fremling10, J. R. Maund11, S. J. Smartt12, T. Krühler13, J. C. A. Miller-Jones14, P. M. Vreeswijk1, A. Gal-Yam1, P. A. Mazzali15,16, A. De Cia17, D. A. Howell8,18, C. Inserra12, F. Patat17, A. de Ugarte Postigo2,19, O. Yaron1, C. Ashall15, I. Bar1, H. Campbell3,20, T.-W. Chen13, M. Childress21, N. Elias-Rosa22, J. Harmanen23, G. Hosseinzadeh8,18, J. Johansson1, T. Kangas23, E. Kankare12, S. Kim24, H. Kuncarayakti25,26, J. Lyman27, M. R. Magee12, K. Maguire12, D. Malesani2, S. Mattila3,23,28, C. V. McCully8,18, M. Nicholl29, S. Prentice15, C. Romero-Cañizales24,25, S. Schulze24,25, K. W. Smith12, J. Sollerman10, M. Sullivan21, B. E. Tucker30,31, S. Valenti32, J. C. Wheeler33 and D. R. Young12 8 12,13 When a star passes within the tidal radius of a supermassive has a mass >10 M⊙ , a star with the same mass as the Sun black hole, it will be torn apart1. For a star with the mass of the could be disrupted outside the event horizon if the black hole 8 14 Sun (M⊙) and a non-spinning black hole with a mass <10 M⊙, were spinning rapidly . The rapid spin and high black hole the tidal radius lies outside the black hole event horizon2 and mass can explain the high luminosity of this event. -
Rare Superluminous Supernova Shining with Borrowed Energy Source Spotted with the 3.6M DOT Facility an Extremely Bright, Hydrog
Rare superluminous supernova shining with borrowed energy source spotted with the 3.6m DOT facility An extremely bright, hydrogen deficient, fast-evolving supernovae that shines with the energy borrowed from an exotic type of neutron star with an ultra-powerful magnetic field has been spotted by Indian researchers. Deep study of such ancient spatial objects can help probe the mysteries of the early universe. Such type of supernovae called SuperLuminous Supernova (SLSNe) is very rare. This is because they are generally originated from very massive stars (minimum mass limit is more than 25 times to that of the Sun), and the number distribution of such massive stars in our galaxy or in nearby galaxies is sparse. Among them, SLSNe-I has been counted to about 150 entities spectroscopically confirmed so far. These ancient objects are among the least understood SNe because their underlying sources are unclear, and their extremely high peak luminosity is unexplained using the conventional SN power-source model involving Ni56 - Co56 - Fe56 decay. SN 2020ank, which was first discovered by the Zwicky Transient Facility on 2020 January 19, was studied by scientists from Aryabhatta Research Institute of Observational Sciences (ARIES) Nainital, an autonomous research institute under the Department of Science and Technology (DST) Govt. of India from February 2020 and then through the lockdown phase of March and April. The apparent look of the SN was very similar to other objects in the field. However, once the brightness was estimated, it turned out as a very blue object reflecting its brighter character. The team observed it using special arrangements at India’s recently commissioned Devasthal Optical Telescope (DOT-3.6m) along with two other Indian telescopes: Sampurnanand Telescope-1.04m and Himalayan Chandra Telescope-2.0m. -
A Magnetar Model for the Hydrogen-Rich Super-Luminous Supernova Iptf14hls Luc Dessart
A&A 610, L10 (2018) https://doi.org/10.1051/0004-6361/201732402 Astronomy & © ESO 2018 Astrophysics LETTER TO THE EDITOR A magnetar model for the hydrogen-rich super-luminous supernova iPTF14hls Luc Dessart Unidad Mixta Internacional Franco-Chilena de Astronomía (CNRS, UMI 3386), Departamento de Astronomía, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile e-mail: [email protected] Received 2 December 2017 / Accepted 14 January 2018 ABSTRACT Transient surveys have recently revealed the existence of H-rich super-luminous supernovae (SLSN; e.g., iPTF14hls, OGLE-SN14-073) that are characterized by an exceptionally high time-integrated bolometric luminosity, a sustained blue optical color, and Doppler- broadened H I lines at all times. Here, I investigate the effect that a magnetar (with an initial rotational energy of 4 × 1050 erg and 13 field strength of 7 × 10 G) would have on the properties of a typical Type II supernova (SN) ejecta (mass of 13.35 M , kinetic 51 56 energy of 1:32 × 10 erg, 0.077 M of Ni) produced by the terminal explosion of an H-rich blue supergiant star. I present a non-local thermodynamic equilibrium time-dependent radiative transfer simulation of the resulting photometric and spectroscopic evolution from 1 d until 600 d after explosion. With the magnetar power, the model luminosity and brightness are enhanced, the ejecta is hotter and more ionized everywhere, and the spectrum formation region is much more extended. This magnetar-powered SN ejecta reproduces most of the observed properties of SLSN iPTF14hls, including the sustained brightness of −18 mag in the R band, the blue optical color, and the broad H I lines for 600 d. -
Ucalgary 2017 Welbankscamar
University of Calgary PRISM: University of Calgary's Digital Repository Graduate Studies The Vault: Electronic Theses and Dissertations 2017 Photometric and Spectroscopic Signatures of Superluminous Supernova Events The puzzling case of ASASSN-15lh Welbanks Camarena, Luis Carlos Welbanks Camarena, L. C. (2017). Photometric and Spectroscopic Signatures of Superluminous Supernova Events The puzzling case of ASASSN-15lh (Unpublished master's thesis). University of Calgary, Calgary, AB. doi:10.11575/PRISM/27339 http://hdl.handle.net/11023/3972 master thesis University of Calgary graduate students retain copyright ownership and moral rights for their thesis. You may use this material in any way that is permitted by the Copyright Act or through licensing that has been assigned to the document. For uses that are not allowable under copyright legislation or licensing, you are required to seek permission. Downloaded from PRISM: https://prism.ucalgary.ca UNIVERSITY OF CALGARY Photometric and Spectroscopic Signatures of Superluminous Supernova Events The puzzling case of ASASSN-15lh by Luis Carlos Welbanks Camarena A THESIS SUBMITTED TO THE FACULTY OF GRADUATE STUDIES IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF MASTER OF SCIENCE GRADUATE PROGRAM IN PHYSICS AND ASTRONOMY CALGARY, ALBERTA JULY, 2017 c Luis Carlos Welbanks Camarena 2017 Abstract Superluminous supernovae are explosions in the sky that far exceed the luminosity of standard supernova events. Their discovery shattered our understanding of stellar evolution and death. Par- ticularly, the discovery of ASASSN-15lh a monstrous event that pushed some of the astrophysical models to the limit and discarded others. In this thesis, I recount the photometric and spectroscopic signatures of superluminous super- novae, while discussing the limitations and advantages of the models brought forward to explain them. -
Central Engines and Environment of Superluminous Supernovae
Central Engines and Environment of Superluminous Supernovae Blinnikov S.I.1;2;3 1 NIC Kurchatov Inst. ITEP, Moscow 2 SAI, MSU, Moscow 3 Kavli IPMU, Kashiwa with E.Sorokina, K.Nomoto, P. Baklanov, A.Tolstov, E.Kozyreva, M.Potashov, et al. Schloss Ringberg, 26 July 2017 First Superluminous Supernova (SLSN) is discovered in 2006 -21 1994I 1997ef 1998bw -21 -20 56 2002ap Co to 2003jd 56 2007bg -19 Fe 2007bi -20 -18 -19 -17 -16 -18 Absolute magnitude -15 -17 -14 -13 -16 0 50 100 150 200 250 300 350 -20 0 20 40 60 Epoch (days) Superluminous SN of type II Superluminous SN of type I SN2006gy used to be the most luminous SN in 2006, but not now. Now many SNe are discovered even more luminous. The number of Superluminous Supernovae (SLSNe) discovered is growing. The models explaining those events with the minimum energy budget involve multiple ejections of mass in presupernova stars. Mass loss and build-up of envelopes around massive stars are generic features of stellar evolution. Normally, those envelopes are rather diluted, and they do not change significantly the light produced in the majority of supernovae. 2 SLSNe are not equal to Hypernovae Hypernovae are not extremely luminous, but they have high kinetic energy of explosion. Afterglow of GRB130702A with bumps interpreted as a hypernova. Alina Volnova, et al. 2017. Multicolour modelling of SN 2013dx associated with GRB130702A. MNRAS 467, 3500. 3 Our models of LC with STELLA E ≈ 35 foe. First year light ∼ 0:03 foe while for SLSNe it is an order of magnitude larger. -
Progenitors of Gamma-Ray Bursts and Supernovae
Progenitors of Gamma-Ray Bursts and Supernovae Chris Fryer (LANL) Types of supernova and GRBs Engines and their progenitor requirements Massive star progenitors and the circumstellar medium (single vs. binary) Specific examples – What have we learned? Supernova Types • Supernovae are distinguished by spectra and light curves. • Unfortunately, in core- collapse, the dividing lines are more like guidelines. • There are many “stand- outs” among these supernovae (e.g. SN87A). SN types - Rates • Core-collapse (Ib/c, II) SNe make up 75% of all supernovae. • Most Ib/c are Ic supernovae. • Plateau SNe make up most of the type II class. • New classes include Broad Line (tied to GRBs?) and Superluminous Supernova GRB Types • GRBs have been roughly Levan et al. (2013) divided into short/hard and long/ soft bursts. • A new class of ultra-long bursts have been discovered. Core-collapse Supernovae (Type II, Ib/c): Powered by SN Engines the potential energy released in collapse Source of convection (advective acoustic vs. Rayleigh Taylor), energy transport (neutrinos, pressure waves), role of magnetic fields. Massive Star Progenitors (binaries vs. single stars) Thermonuclear Supernovae Ignition site/sites White dwarf (double Degenerate vs. single degenerate) Possible Fates under the Convective Paradigm • Explosion within first ~200 ms, normal supernovae • Explosion delayed, weak supernova, considerable fallback (BH formation – Collapsar type II for rotating systems) • No explosion (BH Formation – Collapsar type I for rotating systems) Supernovae/Hypernovae Nomoto et al. (2003) EK (Jets!) Failed SN? 13M~15M BHAD GRB and Magnetar Engines Massive star Collapse (LGRB, very long GRB), only a very small fraction of massive stars (0.01-0.1% the supernova rate). -
The Life Cycle of the Stars Chart
NAME__________________________________DATE_______________PER________ The Life Cycle of the Stars Chart Refer to the “Life Cycle of the Stars Notes and the following terms to fill in the labels on the chart: Black Hole (Forms after the supernova of a massive star that is more than 5 times the mass of the sun) Black Dwarf Star (The remains of a white dwarf that no longer shines) Blue Supergiant Star (more than 3 times more massive than our sun) Nebula (clouds of interstellar dust and gas) Neutron Star (Forms after the supernova of a massive star. Neutron stars are about 10-20 km in diameter but 1.4 times the mass of sun) Planetary or Ring Nebula (the aftermath of a Red Giant that goes “nova”, which means it expels it outer layers) Red Dwarf Star ( a main sequence star of small size and lower temperature) Red Giant Star ( Forms from sun-like stars that start fusing helium. The star expands and cools to a red giant) Red Supergiant Star (Forms from massive stars that start fusing helium. The star expands and cools to a supergiant) Sun-Like Star (a yellow medium-sized star) Supernova (Occurs after a massive star produces iron which cannot be fused further. The result us a massive explosion) White Dwarf (The left-over core of a red giant that has expelled its outer layers. It may continue to shine for billions of years) Color all stars (except neutron star) the appropriate color with colored pencil or marker. Color nebulas red and orange. Do not color supernovas and black holes. -
Tev Emission from NGC1275 Viewed by SHALON 15 Year Observations V.G
XVI International Symposium on Very High Energy Cosmic Ray Interactions ISVHECRI 2010, Batavia, IL, USA (28 June 2 July 2010) 1 TeV emission from NGC1275 viewed by SHALON 15 year observations V.G. Sinitsyna, S.I. Nikolsky, V.Y. Sinitsyna P.N. Lebedev Physical Institute, Leninsky pr. 53, Moscow, Russia The Perseus cluster of galaxies is one of the best studied clusters due to its proximity and its brightness. It have also been considered as sources of TeV gamma-rays. The new extragalactic source was detected at TeV energies in 1996 using the SHALON telescopic system. This object was identified with NGC 1275, a giant elliptical galaxy lying at the center of the Perseus cluster of galaxies; its image is presented. The maxima of the TeV gamma-ray, X-ray and radio emission coincide with the active nucleus of NGC 1275. But, the X-ray and TeV emission disappears almost completely in the vicinity of the radio lobes. The correlation TeV with X-ray emitting regions was found. The integral gamma-ray flux of NGC1275 is found to be (0.78 ± 0.13) × 10−12cm−2s−1 at energies > 0.8 TeV. Its energy spectrum from 0.8 to 40 TeV can be approximated by the power law with index k = −2.25 ± 0.10. NGC1275 has been also observed by other experiments: Tibet Array (5TeV) and then with Veritas telescope at energies about 300 GeV in 2009. The recent detection by the Fermi LAT of gamma- rays from the NGC1275 makes the observation of the energy E > 100 GeV part of its broadband spectrum particularly interesting. -
A COMPREHENSIVE STUDY of SUPERNOVAE MODELING By
A COMPREHENSIVE STUDY OF SUPERNOVAE MODELING by Chengdong Li BS, University of Science and Technology of China, 2006 MS, University of Pittsburgh, 2007 Submitted to the Graduate Faculty of the Dietrich School of Arts and Sciences in partial fulfillment of the requirements for the degree of Doctor of Philosophy University of Pittsburgh 2013 UNIVERSITY OF PITTSBURGH PHYSICS AND ASTRONOMY DEPARTMENT This dissertation was presented by Chengdong Li It was defended on January 22nd 2013 and approved by John Hillier, Professor, Department of Physics and Astronomy Rupert Croft, Associate Professor, Department of Physics Steven Dytman, Professor, Department of Physics and Astronomy Michael Wood-Vasey, Assistant Professor, Department of Physics and Astronomy Andrew Zentner, Associate Professor, Department of Physics and Astronomy Dissertation Director: John Hillier, Professor, Department of Physics and Astronomy ii Copyright ⃝c by Chengdong Li 2013 iii A COMPREHENSIVE STUDY OF SUPERNOVAE MODELING Chengdong Li, PhD University of Pittsburgh, 2013 The evolution of massive stars, as well as their endpoints as supernovae (SNe), is important both in astrophysics and cosmology. While tremendous progress towards an understanding of SNe has been made, there are still many unanswered questions. The goal of this thesis is to study the evolution of massive stars, both before and after explosion. In the case of SNe, we synthesize supernova light curves and spectra by relaxing two assumptions made in previous investigations with the the radiative transfer code cmfgen, and explore the effects of these two assumptions. Previous studies with cmfgen assumed γ-rays from radioactive decay deposit all energy into heating. However, some of the energy excites and ionizes the medium. -
Superluminous Supernovae 56 I H Neato Ewe Uenv Jcaaddense and Ejecta Supernova Between Interaction the Ni, ⋆ − ∼ · · Ln .Sorokina I
SSRv manuscript No. (will be inserted by the editor) Superluminous supernovae Takashi J. Moriya⋆ · Elena I. Sorokina · Roger A. Chevalier Received: 25 December 2017 / Accepted: 5 March 2018 Abstract Superluminous supernovae are a new class of supernovae that were recognized about a decade ago. Both observational and theoretical progress has been significant in the last decade. In this review, we first briefly summarize the observational properties of superluminous super- novae. We then introduce the three major suggested luminosity sources to explain the huge luminosities of superluminous supernovae, i.e., the nu- clear decay of 56Ni, the interaction between supernova ejecta and dense circumstellar media, and the spin down of magnetars. We compare these models and discuss their strengths and weaknesses. Keywords supernovae · superluminous supernovae · massive stars 1 Introduction Superluminous supernovae (SLSNe) are supernovae (SNe) that become more luminous than ∼ −21 mag in optical. They are more than 1 mag more luminous than broad-line Type Ic SNe, or the so-called “hypernovae,” ⋆ NAOJ Fellow T. J. Moriya Division of Theoretical Astronomy, National Astronomical Observatory of Japan, National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan E-mail: [email protected] E. I. Sorokina Sternberg Astronomical Institute, M.V. Lomonosov Moscow State University, Uni- versitetski pr. 13, 119234 Moscow, Russia E-mail: [email protected] arXiv:1803.01875v2 [astro-ph.HE] 9 Mar 2018 R. A. Chevalier Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325, USA E-mail: [email protected] 2 which have kinetic energy of more than ∼ 1052 erg and are the most lumi- nous among the classical core-collapse SNe. -
Black Hole Central Engine for Ultra-Long Gamma-Ray Burst
DRAFT VERSION OCTOBER 16, 2018 Preprint typeset using LATEX style emulateapj v. 5/2/11 BLACK HOLE CENTRAL ENGINE FOR ULTRA-LONG GAMMA-RAY BURST 111209A AND ITS ASSOCIATED SUPERNOVA 2011KL HE GAO1 ,WEI-HUA LEI2,ZHI-QIANG YOU1 AND WEI XIE2 Draft version October 16, 2018 ABSTRACT Recently, the first association between an ultra-long gamma-ray burst (GRB) and a supernovais reported, i.e., GRB 111209A/SN 2011kl, which enables us to investigate the physics of central engines or even progenitors for ultra-long GRBs. In this paper, we inspect the broad-band data of GRB 111209A/SN 2011kl. The late- time X-ray lightcurve exhibits a GRB 121027A-like fall-back bump, suggesting a black hole central engine. We thus propose a collapsar model with fall-back accretion for GRB 111209A/SN 2011kl. The required model parameters, such as the total mass and radius of the progenitorstar, suggest that the progenitorof GRB 111209A is more likely a Wolf-Rayet star instead of blue supergiant, and the central engine of this ultra-long burst is a black hole. The implications of our results is discussed. Subject headings: accretion, accretion disks - black hole physics - gamma-ray burst: individual (GRB 111209A) 1. INTRODUCTION tized millisecond neutronstar (a magnetar) (Levan et al. 2014; Recently, “ultra-long bursts”, a subclass of gamma-ray Greiner et al. 2015). Research on the physical origin of ultra- bursts (GRBs) with unusually long central engine activity (∼ long GRBs would potentially promote our understanding of hours) compared to typical GRBs (tens of seconds), have been the central engine and progenitor of GRBs.