A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.

Slides:



Advertisements
Similar presentations
Insights from Radio Wavelengths into Supernova Progenitors Laura Chomiuk Jansky Fellow, Michigan State University.
Advertisements

Cosmological measurements with Supernovae Ia
Neutron Stars: Insights into their Formation, Evolution & Structure from their Masses and Radii Feryal Ozel University of Arizona In collaboration with.
Jets in GRBs Tsvi Piran Racah Institute of Physics, The Hebrew University Omer Bromberg, Ehud Nakar Re’em Sari, Franck Genet, Martin Obergaulinger, Eli.
The Flavours of SN II Light Curves Iair (“ya-eer”) Arcavi Advisor: Avishay Gal-Yam.
The Science of Gamma-Ray Bursts: caution, extreme physics at play Bruce Gendre ARTEMIS.
Type Ia Supernovae Progenitors. Type Ia Supernovae Historical defining characteristics: Generally, lack of lines of hydrogen Contain a strong Si II absorption.
Stephen C.-Y. Ng McGill University. Outline Why study supernova? What is a supernova? Why does it explode? The aftermaths --- Supernova remnants Will.
Circumstellar interaction in supernovae Poonam Chandra Royal Military Collage of Canada.
The Deaths of Stars The Southern Crab Nebula (He2-104), a planetary nebula (left), and the Crab Nebula (M1; right), a supernova remnant.
Neutron Stars and Black Holes Please press “1” to test your transmitter.
Supernovae Supernova Remnants Gamma-Ray Bursts. Summary of Post-Main-Sequence Evolution of Stars M > 8 M sun M < 4 M sun Subsequent ignition of nuclear.
2009 July 8 Supernova Remants and Pulsar Wind Nebulae in the Chandra Era 1 Modeling the Dynamical and Radiative Evolution of a Pulsar Wind Nebula inside.
Thermonuclear Supernovae Lifan Wang Texas A&M University Oct 6, 2013.
Neutron Stars and Black Holes
From Progenitor to Afterlife Roger Chevalier SN 1987AHST/SINS.
Raffaella Margutti Harvard – Institute for Theory and Computation On behalf of the Harvard SN forensic team Kyoto2013 What happens when jets barely break.
Low-luminosity GRBs and Relativistic shock breakouts Ehud Nakar Tel Aviv University Omer Bromberg Tsvi Piran Re’em Sari 2nd EUL Workshop on Gamma-Ray Bursts.
Low-luminosity GRBs and Relativistic shock breakouts Ehud Nakar Tel Aviv University Omer Bromberg Re’em Sari Tsvi Piran GRBs in the Era of Rapid Follow-up.
Supernovae from Massive Stars: light curves and spectral evolution Bruno Leibundgut ESO.
Gamma-Ray Burst Optical Observations with AST3 Xue-Feng Wu Xue-Feng Wu Chinese Center for Antarctic Astronomy, Chinese Center for Antarctic Astronomy,
Neutron Star Formation and the Supernova Engine Bounce Masses Mass at Explosion Fallback.
Supernovae of type Ia: the final fate of low mass stars in close bynary systems Oscar Straniero INAF – Oss. Astr. di Collurania (TE)
Engine-Driven Supernovae Alicia M. Soderberg Caltech Astronomy Dept. Zwicky Supernova Workshop January
Gamma-ray bursts Discovered in 1968 by Vela spy satellites
XRF associated with SN 2006aj Nature, Val 442 Aug.31 issues Campana et al. p.1008 Pian et al. P Soderberg et al. p.1014 Paolo et al. p.1018.
NASA's Chandra Sees Brightest Supernova Ever N. Smith et al. 2007, astro-ph/ v2.
A Radio Perspective on the GRB-SN Connection Alicia Soderberg May 25, 2005 – Zwicky Conference.
Kick of neutron stars as a possible mechanism for gamma-ray bursts Yong-Feng Huang Department of Astronomy, Nanjing University.
Physics 777 Plasma Physics and Magnetohydrodynamics (MHD) Instructor: Gregory Fleishman Lecture 13. Astrophysical Plasmas 02 December 2008.
G.E. Romero Instituto Aregntino de Radioastronomía (IAR), Facultad de Ciencias Astronómicas y Geofísicas, University of La Plata, Argentina.
The Ultra-luminous X-Ray Sources Near the Center of M82 NTHU 10/18/2007 Yi-Jung Yang.
(Informal) workshop - Ferrara April 2004 SNe. Astrophysical (natural) Explosive Devices Thermonuclear SNe Gravitational collapse C-deflagration He-detonation.
Supernovae Historically: “new stars” in sky Seen in 1006, 1054, 1181, 1572, 1604, 1680 SN 1054 visible in daytime sky for many months (Chinese records)
Wide field X (& UV ?) Identify transients, distribute alerts Candidate X (&UV)-transients SN breakouts XRF ’ s LL GRBs Unknown (eg BH-Stellar disruptions)?
Gamma Ray Bursts and LIGO Emelie Harstad University of Oregon HEP Group Meeting Aug 6, 2007.
A Broader Perspective on the GRB-SN Connection Alicia M. Soderberg Caltech Schramm Symposium, Dec
Supernovae Oscar Straniero INAF – Oss. Astr. di Collurania (TE)
SN Ia: Blown to Smithereens (Röpke and Hillebrandt 2005) Nick Cowan UW Astronomy March 2005 Nick Cowan UW Astronomy March 2005.
Type Ia Supernovae: standard candles? Roger Chevalier.
Supernovas Supernova = When gravity wins… core collapses and a star explodes. Two main types: Type I and Type II Relatively rare: occur every years.
Gamma-Ray Bursts and Supernovae Tsinghua Transient Workshop 8 Nov 2012 Elena Pian INAF-Trieste Astronomical Observatory, Italy & Scuola Normale Superiore.
Supernovae and Gamma-Ray Bursts. Summary of Post-Main-Sequence Evolution of Stars M > 8 M sun M < 4 M sun Subsequent ignition of nuclear reactions involving.
The Supernova Rate with WFXT M. Della Valle INAF-Napoli SN 1994D P. Rosati, M. Paolillo D. De Martino, S. Campana, L. Stella +
QSO -  QSO -  GRB ANALOGY HAVE THE SAME 3 BASIC INGREEDIENTS (M. & Luis Rodriguez, S&T 2002) AN UNIVERSAL MAGNETO-HYDRODINAMIC MECHANISM FOR JETS ?
Recent Observations of GRB-Supernovae Bethany Elisa Cobb The George Washington University IAU Symposium 279 March 13, 2012.
COLLABORATORS: Dale Frail, Derek Fox, Shri Kulkarni, Fiona Harrisson, Edo Berger, Douglas Bock, Brad Cenko and Mansi Kasliwal.
Dec. 6, Review: >8Msun stars become Type II SNe As nuclear burning proceeds to, finally, burning Silicon (Si) into iron (Fe), catastrophe looms.
A panchromatic view of the restless SN2009ip reveals the explosive ejection of a massive stellar envelope.
Different Kinds of “Novae” I. Super Novae Type Ia: No hydrogen, CO WD deflagration --> detonation Type Ia: No hydrogen, CO WD deflagration --> detonation.
BH Astrophys. Ch3.6. Outline 1. Some basic knowledge about GRBs 2. Long Gamma Ray Bursts (LGRBs) - Why so luminous? - What’s the geometry? - The life.
Gamma-Ray Bursts Energy problem and beaming * Mergers versus collapsars GRB host galaxies and locations within galaxy Supernova connection Fireball model.
Gamma-Ray Bursts: Open Questions and Looking Forward Ehud Nakar Tel-Aviv University 2009 Fermi Symposium Nov. 3, 2009.
Radio and X-ray observations of SN 2009ip Poonam Chandra National Centre for Radio Astrophysics January 4, 2013 Collaborators: Raffaella Margutti (Harvard),
Dec. 11, Review Neutron Stars(NSs) and SNR (Crab Nebula…) and then on to BHs… SN-II produce a NS for massive stars in approx. range 8-15Msun; and.
Feedback Observations and Simulations of Elliptical Galaxies –Daniel Wang, Shikui Tang, Yu Lu, Houjun Mo (UMASS) –Mordecai Mac-Low (AMNH) –Ryan Joung (Princeton)
Progenitor stars of supernovae Poonam Chandra Royal Military College of Canada.
X-ray study of a nearby nuclear X-ray study of a nearby nuclear starburst and a nearby AGN starburst and a nearby AGN Roberto Soria (UCL) Mat Page, Kinwah.
Hyperaccreting Disks around Neutrons Stars and Magnetars for GRBs: Neutrino Annihilation and Strong Magnetic Fields Dong Zhang (Ohio State) Zi-Gao Dai.
9 May 2013: New Moon Image: May 2012 annular eclipse, Monument Valley AZ.
The Vigorous Afterlife of Massive Stars Kristen Menou Institut d’Astrophysique de Paris (IAP)
The Exceptional GRB/XRF and its Associated SN 2006aj Jinsong Deng National Astronomical Observatories of China.
Gamma-Ray Bursts. Short (sub-second to minutes) flashes of gamma- rays, for ~ 30 years not associated with any counterparts in other wavelength bands.
Active Galaxies Galaxies with extremely violent energy release in their nuclei (pl. of nucleus). → “Active Galactic Nuclei” (= AGN) Up to many thousand.
Gamma-Ray Bursts Please press “1” to test your transmitter.
Supernova Interaction with Dense Mass Loss
Short-Duration Gamma-Ray Burst Central Engines
DVU, Playa de Carmen, Mexico Dec. 12, 2017
RADIO EMISSION FROM SNe & GRBs, AND THE NEED FOR SKA
GRB-Supernova observations: State of the art
Presentation transcript:

A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing

Margutti +13, +14; Kamble +13; Soderberg +06, +10 Energy partitioning SNe are an OPTICAL phenomenon erg OPTICAL erg X-rays/Radio

RADIATION from the REMNANT X-rays from Supernovae Log Time Log Lx < hr SHOCK BREAK OUT (R exploding star) Δt≈ 2ms T≈250 keV E≈ erg Δt≈ hrs T0+5hrs) T≈ X-rays E≈ erg L~10 44 erg/s SHOCK INTERACTION w. COMPANION (R and distance of the companion) Kasen +10 < several hrs SHOCK/JET INTERACTION w. the MEDIUM (mass-loss of the progenitor) > 10 years MASS-LOSS PROGENITORS SOURCE of ENERGY

…BUT…

RADIATION from the REMNANT X-rays from Supernovae Log Time Log Lx < hr < several hrs SHOCK/JET INTERACTION w. the MEDIUM (mass-loss of the progenitor) > 10 years MASS-LOSS SHOCK BREAK OUT (R exploding star) Δt≈ 2ms T≈250 keV E≈ erg Δt≈ hrs T0+5hrs) T≈ X-rays E≈ erg L~10 44 erg/s SHOCK INTERACTION w. COMPANION (R and distance of the companion) Kasen +10 PROGENITORS SOURCE of ENERGY

MASS-LOSS Direct probe of EVOLUTION, Indirect probe of PROGENITORS SOURCE of ENERGY Explosion Mechanism Type Ia SNe, Type Iax, Type Ibc, Type IIb, Strongly interacting SNe, Relativistic SNe, GRB-SNe, Super-Luminous SNe Type Ia Relativistic SNe

The PROBLEM Progenitor System “…The end is where we start from…” The Little Gidding by T. S. Eliot Type Ia SN explosion ?

WD ? Double Degenerate (DD) Single Degenerate (SD) Exploding star HIGH-density environment DIRTY LOW-density environment CLEAN “Traditional” way of thinking

Margutti R≈10 16 cm SD systems with STEADY mass- loss

Margutti +14 Ruled Out

… “It’s black cats in dark rooms”… (S. Firenstein)

Margutti +12; +14

Margutti +14 … “Its black cats in dark rooms… and there may be no cat in the room” (S. Firenstein) Symbiotic systems with stable mass-loss are ruled out

MASS-LOSS Type Ia SOURCE of ENERGY Relativistic SNe Symbiotic systems with stable mass- loss are ruled out TAKE AWAY MESSAGES:

Margutti+14 Radio Rel SNe Faint GRBs In the Radio/optical relativistic SNe looks the same as faint GRBs X-rays Relativistic SNe are an intrinsically different class of explosions

GRB Faint GRB Relativistic SN Fully successful jet break out Barely successful Barely failed There is some good in every person Jet SN

MASS-LOSS Type Ia Symbiotic systems with stable mass- loss are ruled out TAKE AWAY MESSAGES: SOURCE of ENERGY Relativistic SNe Jets might be ubiquitous

X-rays from Supernovae Log Time < few hr> 10 years SHOCK BREAK OUT (R exploding star) SHOCK INTERACTION w. COMPANION (R and distance of the companion) SHOCK/JET INTERACTION w. the MEDIUM (mass-loss of the progenitor) RADIATION from the REMNANT (accreting BH, MAGNETAR) Successful JET PRESENTPAST FUTURE Very early observations (DIFFICULT) Faint (DIFFICULT) RADIATION from the REMNANT in engine driven SNe days Log Lx COOLING ENVELOPE (R envelope) ACCRETION onto the progenitor

SN1994I SN2002ap GRB/SNe “Standard”, envelope stripped SN IbcHydrogen-poor Super Luminous SNe (M<-21) (e.g. Gal-Yam 2012) 7x10 43 erg/s Super-Luminous SNe

MASS-LOSS Type Ia SOURCE of ENERGY Relativistic SNe Symbiotic systems with stable mass- loss are ruled out TAKE AWAY MESSAGES: Jets might be ubiquitous Super-Lum I

X-rays from Supernovae Log Time < few hr > 10 years SHOCK BREAK OUT (R exploding star) SHOCK INTERACTION w. COMPANION (R and distance of the companion) SHOCK/JET INTERACTION w. the MEDIUM (mass-loss of the progenitor) RADIATION from the REMNANT (accreting BH, MAGNETAR) Successful JET PRESENTPAST FUTURE Very early observations (DIFFICULT) Faint (DIFFICULT) RADIATION from the REMNANT in engine driven SNe days Log Lx COOLING ENVELOPE (R envelope) ACCRETION onto the progenitor FUTURE Thanks to the Chandra Team!! MASS-LOSS PROGENITORS SOURCE of ENERGY < hours

BACK UP

There is some good in every person Barely successful jet break out Consistent with hydrodynamical explosion (No need for a jet/engine) Barely failed jet break out Fully successful jet break out Jet SN

Type Ia SN2014J Host Galaxy: M82, D=3.5 Mpc Explosion image Margutti +14 Chandra X-ray images