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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. -
Introduction to Astronomy from Darkness to Blazing Glory
Introduction to Astronomy From Darkness to Blazing Glory Published by JAS Educational Publications Copyright Pending 2010 JAS Educational Publications All rights reserved. Including the right of reproduction in whole or in part in any form. Second Edition Author: Jeffrey Wright Scott Photographs and Diagrams: Credit NASA, Jet Propulsion Laboratory, USGS, NOAA, Aames Research Center JAS Educational Publications 2601 Oakdale Road, H2 P.O. Box 197 Modesto California 95355 1-888-586-6252 Website: http://.Introastro.com Printing by Minuteman Press, Berkley, California ISBN 978-0-9827200-0-4 1 Introduction to Astronomy From Darkness to Blazing Glory The moon Titan is in the forefront with the moon Tethys behind it. These are two of many of Saturn’s moons Credit: Cassini Imaging Team, ISS, JPL, ESA, NASA 2 Introduction to Astronomy Contents in Brief Chapter 1: Astronomy Basics: Pages 1 – 6 Workbook Pages 1 - 2 Chapter 2: Time: Pages 7 - 10 Workbook Pages 3 - 4 Chapter 3: Solar System Overview: Pages 11 - 14 Workbook Pages 5 - 8 Chapter 4: Our Sun: Pages 15 - 20 Workbook Pages 9 - 16 Chapter 5: The Terrestrial Planets: Page 21 - 39 Workbook Pages 17 - 36 Mercury: Pages 22 - 23 Venus: Pages 24 - 25 Earth: Pages 25 - 34 Mars: Pages 34 - 39 Chapter 6: Outer, Dwarf and Exoplanets Pages: 41-54 Workbook Pages 37 - 48 Jupiter: Pages 41 - 42 Saturn: Pages 42 - 44 Uranus: Pages 44 - 45 Neptune: Pages 45 - 46 Dwarf Planets, Plutoids and Exoplanets: Pages 47 -54 3 Chapter 7: The Moons: Pages: 55 - 66 Workbook Pages 49 - 56 Chapter 8: Rocks and Ice: -
• Classifying Stars: HR Diagram • Luminosity, Radius, and Temperature • “Vogt-Russell” Theorem • Main Sequence • Evolution on the HR Diagram
Stars • Classifying stars: HR diagram • Luminosity, radius, and temperature • “Vogt-Russell” theorem • Main sequence • Evolution on the HR diagram Classifying stars • We now have two properties of stars that we can measure: – Luminosity – Color/surface temperature • Using these two characteristics has proved extraordinarily effective in understanding the properties of stars – the Hertzsprung- Russell (HR) diagram If we plot lots of stars on the HR diagram, they fall into groups These groups indicate types of stars, or stages in the evolution of stars Luminosity classes • Class Ia,b : Supergiant • Class II: Bright giant • Class III: Giant • Class IV: Sub-giant • Class V: Dwarf The Sun is a G2 V star Luminosity versus radius and temperature A B R = R R = 2 RSun Sun T = T T = TSun Sun Which star is more luminous? Luminosity versus radius and temperature A B R = R R = 2 RSun Sun T = T T = TSun Sun • Each cm2 of each surface emits the same amount of radiation. • The larger stars emits more radiation because it has a larger surface. It emits 4 times as much radiation. Luminosity versus radius and temperature A1 B R = RSun R = RSun T = TSun T = 2TSun Which star is more luminous? The hotter star is more luminous. Luminosity varies as T4 (Stefan-Boltzmann Law) Luminosity Law 2 4 LA = RATA 2 4 LB RBTB 1 2 If star A is 2 times as hot as star B, and the same radius, then it will be 24 = 16 times as luminous. From a star's luminosity and temperature, we can calculate the radius. -
The Metallicity-Luminosity Relationship of Dwarf Irregular Galaxies
A&A 399, 63–76 (2003) Astronomy DOI: 10.1051/0004-6361:20021748 & c ESO 2003 Astrophysics The metallicity-luminosity relationship of dwarf irregular galaxies II. A new approach A. M. Hidalgo-G´amez1,,F.J.S´anchez-Salcedo2, and K. Olofsson1 1 Astronomiska observatoriet, Box 515, 751 20 Uppsala, Sweden e-mail: [email protected], [email protected] 2 Instituto de Astronom´ıa-UNAM, Ciudad Universitaria, Apt. Postal 70 264, C.P. 04510, Mexico City, Mexico e-mail: [email protected] Received 21 June 2001 / Accepted 21 November 2002 Abstract. The nature of a possible correlation between metallicity and luminosity for dwarf irregular galaxies, including those with the highest luminosities, has been explored using simple chemical evolutionary models. Our models depend on a set of free parameters in order to include infall and outflows of gas and covering a broad variety of physical situations. Given a fixed set of parameters, a non-linear correlation between the oxygen abundance and the luminosity may be established. This would be the case if an effective self–regulating mechanism between the accretion of mass and the wind energized by the star formation could lead to the same parameters for all the dwarf irregular galaxies. In the case that these parameters were distributed in a random manner from galaxy to galaxy, a significant scatter in the metallicity–luminosity diagram is expected. Comparing with observations, we show that only variations of the stellar mass–to–light ratio are sufficient to explain the observed scattering and, therefore, the action of a mechanism of self–regulation cannot be ruled out. -
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. -
How Supernovae Became the Basis of Observational Cosmology
Journal of Astronomical History and Heritage, 19(2), 203–215 (2016). HOW SUPERNOVAE BECAME THE BASIS OF OBSERVATIONAL COSMOLOGY Maria Victorovna Pruzhinskaya Laboratoire de Physique Corpusculaire, Université Clermont Auvergne, Université Blaise Pascal, CNRS/IN2P3, Clermont-Ferrand, France; and Sternberg Astronomical Institute of Lomonosov Moscow State University, 119991, Moscow, Universitetsky prospect 13, Russia. Email: [email protected] and Sergey Mikhailovich Lisakov Laboratoire Lagrange, UMR7293, Université Nice Sophia-Antipolis, Observatoire de la Côte d’Azur, Boulevard de l'Observatoire, CS 34229, Nice, France. Email: [email protected] Abstract: This paper is dedicated to the discovery of one of the most important relationships in supernova cosmology—the relation between the peak luminosity of Type Ia supernovae and their luminosity decline rate after maximum light. The history of this relationship is quite long and interesting. The relationship was independently discovered by the American statistician and astronomer Bert Woodard Rust and the Soviet astronomer Yury Pavlovich Pskovskii in the 1970s. Using a limited sample of Type I supernovae they were able to show that the brighter the supernova is, the slower its luminosity declines after maximum. Only with the appearance of CCD cameras could Mark Phillips re-inspect this relationship on a new level of accuracy using a better sample of supernovae. His investigations confirmed the idea proposed earlier by Rust and Pskovskii. Keywords: supernovae, Pskovskii, Rust 1 INTRODUCTION However, from the moment that Albert Einstein (1879–1955; Whittaker, 1955) introduced into the In 1998–1999 astronomers discovered the accel- equations of the General Theory of Relativity a erating expansion of the Universe through the cosmological constant until the discovery of the observations of very far standard candles (for accelerating expansion of the Universe, nearly a review see Lipunov and Chernin, 2012). -
PHAS 1102 Physics of the Universe 3 – Magnitudes and Distances
PHAS 1102 Physics of the Universe 3 – Magnitudes and distances Brightness of Stars • Luminosity – amount of energy emitted per second – not the same as how much we observe! • We observe a star’s apparent brightness – Depends on: • luminosity • distance – Brightness decreases as 1/r2 (as distance r increases) • other dimming effects – dust between us & star Defining magnitudes (1) Thus Pogson formalised the magnitude scale for brightness. This is the brightness that a star appears to have on the sky, thus it is referred to as apparent magnitude. Also – this is the brightness as it appears in our eyes. Our eyes have their own response to light, i.e. they act as a kind of filter, sensitive over a certain wavelength range. This filter is called the visual band and is centred on ~5500 Angstroms. Thus these are apparent visual magnitudes, mv Related to flux, i.e. energy received per unit area per unit time Defining magnitudes (2) For example, if star A has mv=1 and star B has mv=6, then 5 mV(B)-mV(A)=5 and their flux ratio fA/fB = 100 = 2.512 100 = 2.512mv(B)-mv(A) where !mV=1 corresponds to a flux ratio of 1001/5 = 2.512 1 flux(arbitrary units) 1 6 apparent visual magnitude, mv From flux to magnitude So if you know the magnitudes of two stars, you can calculate mv(B)-mv(A) the ratio of their fluxes using fA/fB = 2.512 Conversely, if you know their flux ratio, you can calculate the difference in magnitudes since: 2.512 = 1001/5 log (f /f ) = [m (B)-m (A)] log 2.512 10 A B V V 10 = 102/5 = 101/2.5 mV(B)-mV(A) = !mV = 2.5 log10(fA/fB) To calculate a star’s apparent visual magnitude itself, you need to know the flux for an object at mV=0, then: mS - 0 = mS = 2.5 log10(f0) - 2.5 log10(fS) => mS = - 2.5 log10(fS) + C where C is a constant (‘zero-point’), i.e. -
STELLAR RADIO ASTRONOMY: Probing Stellar Atmospheres from Protostars to Giants
30 Jul 2002 9:10 AR AR166-AA40-07.tex AR166-AA40-07.SGM LaTeX2e(2002/01/18) P1: IKH 10.1146/annurev.astro.40.060401.093806 Annu. Rev. Astron. Astrophys. 2002. 40:217–61 doi: 10.1146/annurev.astro.40.060401.093806 Copyright c 2002 by Annual Reviews. All rights reserved STELLAR RADIO ASTRONOMY: Probing Stellar Atmospheres from Protostars to Giants Manuel Gudel¨ Paul Scherrer Institut, Wurenlingen¨ & Villigen, CH-5232 Villigen PSI, Switzerland; email: [email protected] Key Words radio stars, coronae, stellar winds, high-energy particles, nonthermal radiation, magnetic fields ■ Abstract Radio astronomy has provided evidence for the presence of ionized atmospheres around almost all classes of nondegenerate stars. Magnetically confined coronae dominate in the cool half of the Hertzsprung-Russell diagram. Their radio emission is predominantly of nonthermal origin and has been identified as gyrosyn- chrotron radiation from mildly relativistic electrons, apart from some coherent emission mechanisms. Ionized winds are found in hot stars and in red giants. They are detected through their thermal, optically thick radiation, but synchrotron emission has been found in many systems as well. The latter is emitted presumably by shock-accelerated electrons in weak magnetic fields in the outer wind regions. Radio emission is also frequently detected in pre–main sequence stars and protostars and has recently been discovered in brown dwarfs. This review summarizes the radio view of the atmospheres of nondegenerate stars, focusing on energy release physics in cool coronal stars, wind phenomenology in hot stars and cool giants, and emission observed from young and forming stars. Eines habe ich in einem langen Leben gelernt, namlich,¨ dass unsere ganze Wissenschaft, an den Dingen gemessen, von kindlicher Primitivitat¨ ist—und doch ist es das Kostlichste,¨ was wir haben. -
Part 2 – Brightness of the Stars
5th Grade Curriculum Space Systems: Stars and the Solar System An electronic copy of this lesson in color that can be edited is available at the website below, if you click on Soonertarium Curriculum Materials and login in as a guest. The password is “soonertarium”. http://moodle.norman.k12.ok.us/course/index.php?categoryid=16 PART 2 – BRIGHTNESS OF THE STARS -PRELIMINARY MATH BACKGROUND: Students may need to review place values since this lesson uses numbers in the hundred thousands. There are two website links to online education games to review place values in the section. -ACTIVITY - HOW MUCH BIGGER IS ONE NUMBER THAN ANOTHER NUMBER? This activity involves having students listen to the sound that different powers of 10 of BBs makes in a pan, and dividing large groups into smaller groups so that students get a sense for what it means to say that 1,000 is 10 times bigger than 100. Astronomy deals with many big numbers, and so it is important for students to have a sense of what these numbers mean so that they can compare large distances and big luminosities. -ACTIVITY – WHICH STARS ARE THE BRIGHTEST IN THE SKY? This activity involves introducing the concepts of luminosity and apparent magnitude of stars. The constellation Canis Major was chosen as an example because Sirius has a much smaller luminosity but a much bigger apparent magnitude than the other stars in the constellation, which leads to the question what else effects the brightness of a star in the sky. -ACTIVITY – HOW DOES LOCATION AFFECT THE BRIGHTNESS OF STARS? This activity involves having the students test how distance effects apparent magnitude by having them shine flashlights at styrene balls at different distances. -
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. -
• Flux and Luminosity • Brightness of Stars • Spectrum of Light • Temperature and Color/Spectrum • How the Eye Sees Color
Stars • Flux and luminosity • Brightness of stars • Spectrum of light • Temperature and color/spectrum • How the eye sees color Which is of these part of the Sun is the coolest? A) Core B) Radiative zone C) Convective zone D) Photosphere E) Chromosphere Flux and luminosity • Luminosity - A star produces light – the total amount of energy that a star puts out as light each second is called its Luminosity. • Flux - If we have a light detector (eye, camera, telescope) we can measure the light produced by the star – the total amount of energy intercepted by the detector divided by the area of the detector is called the Flux. Flux and luminosity • To find the luminosity, we take a shell which completely encloses the star and measure all the light passing through the shell • To find the flux, we take our detector at some particular distance from the star and measure the light passing only through the detector. How bright a star looks to us is determined by its flux, not its luminosity. Brightness = Flux. Flux and luminosity • Flux decreases as we get farther from the star – like 1/distance2 • Mathematically, if we have two stars A and B Flux Luminosity Distance 2 A = A B Flux B Luminosity B Distance A Distance-Luminosity relation: Which star appears brighter to the observer? Star B 2L L d Star A 2d Flux and luminosity Luminosity A Distance B 1 =2 = LuminosityB Distance A 2 Flux Luminosity Distance 2 A = A B Flux B Luminosity B DistanceA 1 2 1 1 =2 =2 = Flux = 2×Flux 2 4 2 B A Brightness of stars • Ptolemy (150 A.D.) grouped stars into 6 `magnitude’ groups according to how bright they looked to his eye. -
HR Diagram You Know the Size of the Star
1 Lecture 26 The Hertzsprung- Russell Diagram January 13b, 2014 2 Hertzsprung-Russell Diagram • Hertzsprung and Russell found a correlation between luminosity and spectral type (temperature) Hot, bright stars 10000 100 Sun Luminosity 1 (Solar units) 0.01 Cool, dim stars 0.0001 Main Sequence hot O B A F G K M cooler 3 4 • Most stars (~90%) are on the main sequence – The greater the temperature, the more luminous the star – M type stars are the most common. – O type stars are the least common. 5 Sizes of Stars • Size of star is related to the temperature and the luminosity by: Luminosity Temperature42 Radius LTR424 – If you know the position on HR diagram you know the size of the star. 6 A star is twice as luminous as the Sun and has twice the surface temperature. What is its radius relative to the Sun’s radius? A. Rstar/RSun = 4.0 B. Rstar/RSun = 2.8 C. Rstar/RSun = 0.5 D. Rstar/RSun = 0.35 7 A star is twice as luminous as the Sun and has twice the surface temperature. What is its radius relative to the Sun’s radius? LTRRLT44 2 4 4 4 4 RLTstarLTstar4 star star Sun RLT4 SunLTSun4 Sun Sun star 4 21 0.35 12 8 100 R 10 R 10000 Supergiants 100 1 R Sun Luminosity 1 Giants (Solar units) 0.01 Cool, dim stars White 0.0001 Dwarfs 0.1 R Main Sequence 0.01 R hotter O B A F G K M cooler Spectral Classification 9 • Supergiants -- cool, bright, red, large stars • Giants -- cool, bright red, less large stars • Main Sequence -- spans range from hot, bright stars to cool, dim stars.