Supernova Remnant - University of Manitobahome.cc.umanitoba.ca/~umchan69/supernovaremenant.pdf · Evidence for super fluidity in the core. Cassiopeia A Background Information •The

Supernova Remnant

Kepler’s Supernova RemnantPhoto Credit: NASA/CXC/NCSU/M.Burkey et al;

Kirsten Chan

Definitions

• Supernova: Explosive death of a star, caused by onset of nuclear burning (Type 1) or an enormously energetic shock (Type 2)

• Supernova Remnant: The scattered glowing remains from a supernova

(Chaisson et al. 2005)

Formation of Supernova Remnant

• When a supernova explosion occurs, energy is released as– Energetic neutrinos (majority)

– Kinetic Energy

• The kinetic energy accelerates through stellar material– Causes shock waves to plows outwards into

interstellar medium

• Interstellar medium gets enriched

• Expanding/additional material from blast travels to interstellar medium, and Supernova Remnants are formed

(hearsarc.gsfc.nasa.gov/docs/objects/snrs/snrstext.html)

Types of Supernova Remnants

• Shell Type

– Nothing in the center (ring-like structure)

Supernova Remnant E0102-72Photo credit: NASA/CXC/SAO

(Germany, et al. 1999)

• Crab-like (aka. Plerions)

– Pulsar in the center (blob-like shape)

Supernova Remnant: Crab NebulaPhoto Credit: Malin/Pasachoff/Caltech (Germany, et al. 1999)

• Composite Types

– Mix between Shell and Crab-like

Supernova Remnant IC 433Photo Credit: Jonathan Keohane (Germany, et al. 1999)

Article #1: Cooling neutron star in the Cassiopeia A supernova remnant:

Evidence for super fluidity in the core

Cassiopeia A Background Information

• The one of the youngest supernova remnant in the Milky Way Galaxy

• Approx 11 000 light years away

• Approx 27 light years across

Cassiopeia APhoto Credit: NASA/CXC/UNAM/Ioffe/D.Page,P.Shternin et al

(Hwang et al. 2012)

Approx 330 year old Neutron StarContains

Carbon Atmosphere

Declining surface temperature

• After a 10 year Chandra observation– Studies concludes to ~4% temperature decline

• Declining surface temperature is explained by the neutrons star core becomes superfluid– Produce a splash of neutrino emission due to cooper

pair formation

(Shternin et al. 2011)

Press Article: NASA’s Chandra Finds New Evidence on Origin of Supernovas

Tycho Background Information

• Supernova remnant of Tycho was discovered in 1572

• Estimated distance ~ 13 000 light years

• Estimated Size: ~20 light years

Supernova Remnant TychoPhoto Credit: NASA/CXC/Chinese Academy of Science/ F.Luet al

(Eriksen, et al. 2011)

• Researchers study remnant of supernova Tycho

• In x-ray emission of the supernova remnant, found an arc• This supports that shock waves created the arc

• Understanding Type 1a supernovas

• Properties of x-ray arc was able to determine

– Separation: 1/10 of distance from earth to sun

– Orbital Period: 5 days

(CXC 2011)

Article #2: Supernova Evolution in an Interstellar Medium with Evaporating Clouds

• Three standard stages of expanding supernova remnants

– Free Expansion Stage

– Adiabatic

– Radiactive Phase

Stages of Expansion

(White at al. 1991)

• Mathematical models of evolution of a supernova remnant expansion in a cloudy interstellar medium

• Detailed calculations of Supernova Remnant Expansion in Cloudy Interstellar Medium

– X-ray, infrared, optical luminosities

(White et al. 1991)

Summary

– Formation

– Classification Types

– Supernova Expansion

– Cassiopeia A Neutron’s Star

– Supernova Evolution in Interstellar Medium with Evaporating Cloud

– Tycho Supernova Remnant

Work Cited Chaisson E, McMillan S. 2011. Astronomy Today. 7th ed. San Francisco, CA. Pearson Education

Inc.

CXC. 2011. NASA’S Chandra finds new Evidence on Origin of Supernovas. Chandra X-Ray Observatory. NASA. chandra.harvard.edu/press/11_releases/press_042611.html

CXC. 2011. Tycho’s Supernova Remnant: Exploding Stars and Stripes. Chandra X-Ray Observatory. NASA. chandra.harvard.edu/photo/2011/tycho/

CXC. 2012. Cassiopeia A: A Star Explodes and Turns Inside Out. Chandra X-Ray Observatory. NASA. chandra.harvard.edu/photo/2012/casa/

DoITPoMS. 2013. Cooper Pair Formation. University of Cambridge. www.doitpoms.ac.uk/tlplib/superconductivity/cooper.php

Germany L, Proctor R, Fluke C, Gaztelu A, Mackie G, et al. 1999. Supernova Remnant Type. The SAO Encyclopedia of Astronomy. Swinburne University of Technology. astronomy.xwin.edu.au/cms/astro/cosmos/s/Supernova+Remnant+Type

Shternin P, Yakovlev D, Heinke C, Ho W, Patnaude D. 2011. Cooling neutron star in the Cassiopeia A supernova remnant: evidence for superfluidity in the core. MNRAS. 412:108-112

White R, Long K. 1991. Supernova Remnant Evolution in an Interstellar Medium with Evaporating Clouds. ApJ. 373:543-555

Introduction to Supernova Remnants. heasarc.gsfc.nasa.gov/docs/objects/snrs/snrstext.html**Note: Other information is currently unavailable due to website shutdown