Dr. Kari Frank (Pennsylvania State University) Supernova 1987A · ViewSpace –Supernova 1987A: Three Decades of Explosive Revelations NASA Press-Releases: 2017 –The Dawn of a New

Supernova 1987A:

The Supernova of a Lifetime

Dr. Kari Frank (Pennsylvania State University)

Dr. Steven Boggs (UC San Diego)

Dr. Robert Kirshner (Harvard University; Gordon and

Betty Moore Foundation)

Kimberly Arcand (Chandra/SAO)

Facilitator: Brandon Lawton (STScI)

Science Briefing

April 13, 2017

Additional Resources

http://nasawavelength.org/list/1728

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Videos:

Hubble Chronicles Brightening of Ring around an Exploded Star

ViewSpace – Supernova 1987A: Three Decades of Explosive

Revelations

NASA Press-Releases:

2017 – The Dawn of a New Era for Supernova 1987A

2015 – Star Explosion is Lopsided, Finds NASA’s NuSTAR

Featured Activities:

3D Printing the X-Ray Universe: SN 1987A

NASA 3D Resources

How to Build a Galaxy

Recoloring the Universe with Pencil Code

Additional Activities:

Supernova! Outreach Toolkit

Stellar Evolution: Our Cosmic Connection

Supernova Explosions

The Crawl of the Crab

Universe Discovery Guides – December

Astro101 Slidesets: From Supernovas to Planets

SN 1987A with X-ray Vision

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Kari A. FrankPennsylvania State University

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SN 1987AThe opportunity of a lifetime

• First visible nearby supernova in 400 years!• February 23, 1987• Large Magellanic Cloud (Milky Way

satellite galaxy)

• First …• Progenitor star identified• Observed with modern telescopes• Observed extensively in non-visible light

(X-ray, radio, infrared, …)• Long-term (decades) monitoring

Australian Astronomical Observatory

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Produces elements used in future generations of stars,

planets, and people.

SN 1987A is the first (and so far only) opportunity see entire process.

Distributes elements for recycling.

A Window into the Past and Future

NASA/CXC/M.Weiss; X-ray: NASA/CXC/GSFC/U.Hwang & J.Laming

LingHK/Shutterstock.com

NASA/CXC/SAO

Massive Star

SupernovaSupernova Remnant

Past Future

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Chandra’s X-ray Vision

• Expanding blast wave heats gas up to millions of degrees, causing it to glow with X-rays

• Chandra has looked at SN 1987A once or twice a year since it launched in 1999

NASA/CXC/NGST

ChandraNuSTAR

Radio Microwave Infrared Optical(Visible) Ultraviolet Gamma-ray

Increasing Energy Increasing Wavelength

X-ray

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The First 17 Years with ChandraReading the star’s history

• The star expelled parts of its outer layers during its life.

• The expanding supernova blast wave lights up this material for us to see with Chandra.

• The denser the material, the brighter the X-rays.

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Phase 1: Dense Clumps1999 - 2003

1 light year

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Phase 2: Dense Clumps + Ring2003 - 2007

1 light year

Expanding at 15 million mph

Expanding at 4 million mph

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Phase 2: Dense Clumps + Ring2003 - 2007

1 light year

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Phase 3: End of Clumps2007 - 2012

1 light year

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Phase 4: Ring Exit2012 - Now

1 light year

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The Picture So Far1999 - 2017

• Ring + clumps structure

• Asymmetric expansion implies lopsided explosion or stellar wind

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Phase 5+: FutureNow - ??

• Probe earlier in star’s history

• Reflected blast wave illuminates shrapnel

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SN 1987AA Window into the Past and Future

Chandra’s X-ray vision has illuminated the last stages

of the star’s life.

NASA/CXC/M.Weiss; X-ray: NASA/CXC/GSFC/U.Hwang & J.Laming

LingHK/Shutterstock.com

NASA/CXC/SAO

Massive Star

SupernovaSupernova Remnant

Past Future

Still more to come!

Lopsided explosion?

The Nuclear Spectroscopic Telescope Array(launched June 2012)

NuSTAR(3-79 keV)

NuSTAR Observations of SN 1987A

Steven Boggs

UC San Diego

Department of Physics17

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Nuclear Gamma RaysStudying the Synthesis and

Distribution of the Elements

Giants (26Al)

• convective shell burning

Stars/Sun (many)

• ion acceleration

• ambient abundances

Interstellar Medium (26Al, 60Fe,...)

• Galactic history of nucleosynthesis

• formation, evolution and death of massive stars

• CR acceleration & interactions

Remnants (44Ti, 26Al, 106Sn)

• structure & dynamics

• ejection of heavy elements

• compact object formation

• discover young remnants

Supernovae (56Ni, 57Ni, 44Ti)

• understand the explosion mechanism

• abundances of synthesized elements

• structure & dynamics of ejecta

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NuSTAR Observations of SN1987A

(Boggs & NuSTAR Team, Science 348, p. 670, 2015)

SN1987A Confirmed Core Collapse Model:• Neutrino burst confirmed collapse of the central core

• 56Co (0.07 M

) and 57Co (0.003) drive UVOIR lightcurve

SM1987A Surprises:• Progenitor was a blue supergiant (20 M

), not red

• 56Co lines emerged months before expected, heavy mixing

NuSTAR SN 1987A Objectives• Constrain models of nucleosynthesis in SN

1987A by measuring the 44Ti production.

• Reveal asymmetries in the explosion mechanism

and further constrain the explosion models

through the 44Ti emission line profile.

• Study HXR emission from remnant.

(NASA, ESA, P. Challis and

R. Kirshner Harvard-Smithsonian CfA)

T1/2 ~60 years

(NASA/JPL-Caltech)

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NuSTAR

Observations

2,596 ksec

2012-2014

26.6 years

(average) after

explosion

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NuSTAR Source & Background Regions

Source region

Background region

Optics cut off ~78.39 keV

Direct background subtraction

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NuSTAR Background-Subtracted 44Ti spectrum

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NuSTAR 44Ti Model Fits - 3 Models

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NuSTAR SN1987A 44Ti Yield

44Ti Yield: (1.5±0.3)×10-4 M

•Consistent with UVOIR lightcurves

•Points towards asymmetric explosion models

67.4 67.5 67.6 67.7 67.8 67.92×

10−

63×

10−

64×

10−

65×

10−

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Flu

x (

pho

ton

s cm

−2 s

−1)

Line Energy (keV)

+

68%

90%

99%

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44Ti Yield Estimates• UVOIR lightcurves and spectra: (0.5-2)×10-4 M

• Theory, network calculations: (0.5-2)×10-4 M

lower = spherically symmetric

higher = larger asymmetries

INTEGRAL yield

(high) Best Fit

(Seitenzahl, Timmes & Magkotsis 2014; includes

good summary of models and theory)

(Motizuki & Kumagai 2004)

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Doppler Broadening: < 4,100 km/s FWHM

•0.56 +0.31/-0.45 keV FWHM @ 68 keV line (corrected)

•NuSTAR energy resolution 0.90 keV FWHM @ 68 keV

•Consistent with 56Co measurements of ~3,000 km/s FWHM

NuSTAR SN1987A 44Ti Doppler Broadening

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NuSTAR SN1987A 44Ti Redshift

67.4 67.5 67.6 67.7 67.8 67.92×

10−

63×

10−

64×

10−

65×

10−

6

Flu

x (

pho

ton

s cm

−2 s

−1)

Line Energy (keV)

+

68%

90%

99%

Net redshift: 1000±400 km/s uncorrected

•0.23±0.09 keV @ 67.87 keV

•NuSTAR calibrated to better than 0.040 keV (3s)

SN 1987A recession: 286.7 km/s (unshocked gas)

•(Gröningsson et al., 2008)

Look-back effect: 50 km/s redhsift

•(Chan & Lingenfelter, 1987)

Corrected redshift: 700±400 km/s redhsift•Significant compared with broadening

•Requires large-scale asymmetry in the explosion

•Confirms earlier 56Co redshifts

•Consistent with the HST results (later)

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(Tueller et al. 1990; Teegarden 1991)

More Surprises!

• 56Ni mixed out to ~3000 km/s FWHM (several times expected).

• ~500 km/s redshift (not blueshift!), but low significance.

56Co Spectra

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UVOIR Lightcurves (late times)

Modeled 44Ti Yield: 1.4×10-4 M

HST Observations

(~4857 d) (Larsson et al. 2011)

44Ti positrons

X-ray heating

from shocks

R band B band

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HST Observations near End of 44Ti-Powered Phase UVOIR spatially coincident with 44Ti ejecta HST-STIS 1999 August 18

HST 2000 June 11

Morphology & kinematics suggest

bipolar structure, elongated N-S[Ca II] l7300 line:

Net redshift (500 – 1700 km/s)

Confusion with [O II] l7320?

(Wang et al. 2002)

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NuSTAR Background-Subtracted 44Ti spectrum

67.87 keV (93.0%) 78.32 keV (96.4%)

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SN1987A Gamma-Ray Measurements Summary

56Co

• confirmation that nuclear decays power supernovae lightcurves

• 56Co Yield: 0.069 M

• early detection of 56Co emission (several months)

• 56Ni mixed out to ~3000 km/s FWHM (several times expected)

• ~500 km/s redshift (not blueshift!), but low significance

57Co

• further confirmation that nuclear decays power supernovae lightcurves

• 57Co Yield: 0.033 M

44Ti

• even further confirmation that nuclear decays power supernovae lightcurves

• study transition from supernovae to supernova remnant (powered by X-ray heating)

• 44Ti Yield: 1.5×10-4 M

• Points towards asymmetric explosion models

• Consistent with most UVOIR lightcurve models

• <4,100 km/s FWHM broadening, consistent with 56Co measurements

• 700 km/s redshift

• Points towards large-scale asymmetry in explosion, single-lobe explosion?

SN 1987A: The Supernova of a Lifetime

Robert P. KirshnerHarvard University

Gordon and Betty Moore Foundation

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SN 1987A: February 23, 1987

Sanduleak -69 202

After Before

A 1987 Space Telescope: International Ultraviolet Explorer

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April 24, 1990

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1990: Faint Object Camera image

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Hubble Chronicles Brightening of Ring around an Exploded Star

You can see the video, here:http://hubblesite.org/video/934/news_release/2017-08

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The rise of the ring!

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Something new: and it isn’t radioactivity!

Many messages!

Figure 9

Evolution of SN1987A and its Equatorial Ring. Top row -- Optical (Fransson et al. 2015). The brightness of the ring has been reduced by a factor 20 to make it

possible to see faint emission from the supernova debris and beyond the ring; Mi ddle Row -- 0.5 - 3 keV X-rays (Frank et al. 2015); Bottom Row -- 9 GHz (Ng.

et al. 2013). 43

ALMA

44

CHANDRA, ALMA & HST

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STIS Slit positions for 3D reconstruction of debris: Larsson et al. (2016)

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Reconstructing 3Dx/t = vx; y/t = vy; z = vrt

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Theoretical Velocity Distributions of 56Ni

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Where is that neutron star?

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Kimberly Arcand, Chandra/SAO, NASA’s Universe of

Learning. [email protected] @kimberlykowal 50

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ASTRONOMY

3D PRINTING IN

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SN 1987a

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chandra.si.edu/photo/2017/sn1987a/

chandra.si.edu/photo/2017/sn1987a/

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Cassiopeia A

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chandra.si.edu/3dprint

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Eta Carinae and

Pillars of Creation

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Eta Carina

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nasa3d.arc.nasa.gov

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How can 3D modeling help experts and non-experts approach the different kinds of objects in space? Learn how 3D models are created with data from NASA's Chandra X-ray Observatory/Smithsonian Astrophysical Observatory and other observatories. Use free CAD software to explore 3D modeling, and receive a 3D printed object after the workshop. The goal is to help learners understand the life cycles of stars and galaxies, while also experimenting with cutting-edge technology through both hardware and software.

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Chandra.si.edu/build

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Working with data from NASA’s Chandra X-ray Observatory and other telescopes on topics from exploded stars, to star-forming regions, to the area around black holes, students learn basic coding (for beginners, no experience required) and follow a video tutorial to create a real world application of science, technology and even art. By enabling students to use real data from NASA’s Chandra X-ray Observatory, along with other astronomical data, this project helps show just how integral coding is in the pursuit of learning about our Universe.

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Chandra.si.edu/code

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Coming Soon: Stellar Origami & Lego builds for 3D SNRs

Kimberly Arcand, Chandra/SAO

NASA’s Universe of Learning

[email protected]

@kimberlykowal

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