Supernovae as Origins of Life
Shigehiro Nagataki
Astrophysical Big Bang Laboratory (ABBL), RIKENInterdisciplinary Theoretical & Mathematical Sciences Program (iTHEMS), RIKEN
Astrophysical Big Bang Group (ABBG), Okinawa Institute of Science and Technology(OIST)ISCO2023, OIST, Okinawa, Japan, 27th Feb.- 3rd Mar. 2023, Presentation Date: 2nd Mar. 2023.

Image: M44, Credit: NAOJ

How can we measure Distances to Stars?

Image: Pleiades,～444 light years.
Credit: NAOJ

First Step: Measure the Distance to the Sun.
A star in the Milky WayθθS = D / tan θSDSEThe Sun. Image Credit: NASA! km.
D～1.5×10
SE
How could we measure it?

SEDSE

Newton’s Law and Radar tell us the Distance
Gravity Force
VEMEDSESunMSEarth! "!""""$"#=##!"#!"
2πD#$ = 𝑉% 𝑇%(𝑇! ～365 days)

Solve
Orbits of Planets
A transit of Venus across the SunVVSun DSV

V

Centrifugal Force

D VE$('()# #!"𝑀% =!
*"#((2π)% 𝐷&'=𝐺𝑇'%(𝑇" ～225 days)

!" cm
D=
Δt×C/2～4×10
Radar EVE

Δt : Round-trip Time of Radio Waves
between Earth & Venus.
C : Speed of Light.
Image Credit: NASAD#$ = D#& + D&$

Human Beings Could Estimate the Distances
w/o Yardstick.
D!" = D!# + D#"
Sun-Earth

Sun-Venus

Venus-Earth#$D!" ～4×10 cm : Radar

#%!"
$&"

=

#%!%
(Kepler’s Third Law)$&%#$

∴ D!" ～ 1.5×10

D&' =(+(,2/3D&)～ 1.38 D&)#$

cm, D!% ～1.1×10cm

Now we can know more about the Sun.
$('()# #!"𝑀% =!
*"#～ 2 × 10-- g.

𝛽～0.26

R#D./°

We could estimate mass of the Sun
w/o weight scale!

R' = D#$ tan 𝛽 ～ 6.9×10!( cm.
We can estimate Luminosity of the Sun, 𝐿) ,as 𝐿) = 4πD*+ , × F ～ 3.8×10-- erg s./ .
F is radiation flux from the Sun [erg/cm! ] at the Earth.

We also know surface temperature of the Sun = 5,800 K, and surface composition (𝑋% ～ 73%, 𝑋%& ～ 25% in mass).
Close to Big Bang Nucleosynthesis.

Furthermore, we also know that the age of the Sun ～ 4.6 billion yrs old from analysis of meteorites.

Standard Solar Model (SSM)
We can construct hydro-static model to satisfy the properties of the Sun (Mass, Radius, Luminosity,Surface temperature & composition, age), using hydrostatic equations with micro-physics (nuclear reactions,Radiation transfer (scatterings, absorption, emission), equation of state). Physics!
4H → ,)He + 2𝑒 - + 2ν& + 3.7×10*. erg.
～ 6 tons of hydrogen is burning to Helium per 1 second.
To support self-gravity of the Sun, Nuclear Reactions by Strong Forceare happening penetrating Coulomb Potential Barrier between
2 protons, followed by Weak Interactions to change protons to neutrons.
All Four Forces in Nature are working efficiently to realize the Sun.

Only X=0.335 is left
at the center!
(𝑇' ～ 1.6×10 K
𝜌' ～ 1.6×10) g cm*+
From HP of Prof. Min S. Yun.
https://people.astro.umass.edu/~myun/teaching/a100_old/longlecture10.html

Figure from ChristensenDalsgaard (2021)

Mass Fraction of Hydrogen
As a Function of Normalized Radius.

Solid: Weymann (1957)
Dashed: ChristensenDalsgaard+ (1996)

Remaining Life-time of the Sun is ～5 billion yrs.
Self-gravity is not supported by nuclear reactionsAnymore.

Log (R(t)/R / )Orbit of the Earth
Each number represents
Mass of the Sun normalized
By the Present Value.
The Sun is losing its mass
by Solar Wind.

RGB Phase(Red Giant Branch)Helium-Shell Burning
To Carbon.

0.9

AGB Phase

0.6

Does it collapse and form a black hole?
No, degenerate pressure of electrons support theSelf-gravity and form a white dwarf (WD).
Sirius A(Asymptotic Giant Branch)Helium Flash in the Core
To Carbon.

0.67
Sirius B (WD)
Sudden Shrink.
Nothing to Burn

Age of the Sun (yr)Figure from SchrÖder and Smith (2008)

Image Credit: NASAFrom HP of Prof. David Taylor

It is considered that stars with (0.07–10) M0end their lives as White Dwarfs.

Supernova Explosions in the Milky Way
Tycho Brahe Observed a Supernova in 1572 near Cassiopeia.
Peak apparent magnitude was ～-4 deg, comparable to Venus.
It became invisible to the naked eye in 1574.

Supernova event rate in the Milky Way is ～ 1 event per Century.
Rare events.

The Painting was done by Camille Flammarion (1880)

Type Ia Supernova in an Extra-Galaxy
Properties of Type Ia Supernovae:・ (Almost) Common Light Curve.
・ Bright Peak Luminosity.
・ Lack of Hydrogen (no hydrogen lines).
・ Strong Si[II] Absorption line.
・ Strong Blends of Fe emission lines.

SN1994D in NGC4251.
～55 Million Light Year from the Earth.
NASA/ESA/Hubble Key Project Team/
High-Z Supernova Search Team

Credit:NASA/JPL-Caltech

S. Perlmutter

B. Schmidt

A. Riess

Normalized Energy Density of Dark Energy

Type Ia Supernovae as the Brightest Standard Candles in the Universe
Figure fromRiess et al. 1998.

Normalized Energy Density of Matter

Noble Prize in Physics 2011 for the Discovery of the AcceleratingExpansion of the Universe through Observations of Distant SupernovaeType Ia Supernovae are Explosions of White Dwarfs•••

Most of Astrophysicists believe that Type Ia Supernovae are Explosions of White Dwarfs (WDs).
The (almost) common light curves are understood by the scale of Chandrasekhar Mass Limit (1938)
and explosive nucleosynthesis of the WD itself (e.g. Hoyle and Fowler 1960).
Theoretical Simulations of Type Ia SN reproduce Observed Light Curves and Spectrum very well.
The Chandrasekhar Mass Limit𝑀)* = 1.45
𝜇& ≡S. Chandrasekhar" "𝑀'+!

Bold: Obs.
Thin: Theory

1234&5 67 82'9&680 :&5 28;< =6923&1234&5 67 &9&'<5680 :&5 28;< =6923&

W. Fowler
WD mass cannot exceed the mass limit.

Nobel Prize in Physics 1983
Subramanyan Chandrasekhar “for his theoretical studies of the physical processes of importance to the structure andevolution of the stars”
William Alfred Fowler “for his theoretical and experimental studies of the nuclear reactions of importance in theformation of the chemical elements in the universe”

Figure from Nomoto et al. 1997

Long Lasting Mystery: How do WDs
exceed the Chandrasekhar Mass Limit?
• Most of Astrophysicists believe that Type Ia Supernovae are Explosions ofWhite Dwarfs (WDs).
• However, no one has identified the progenitor WD(s) that exploded as a TypeIa supernova.
Artistic Image

Artistic Image

Type Ia supernovae are observed
as point sources in extra-galaxies.
Progenitor stars are not identified.

Mass Transfer from a Companion Star?
Single Degenerate Scenario (SD).
NASA/ESA/Hubble Key Project Team/High-Z Supernova Search Team

Image Credit: STFC/David Hardy

Merger of double white dwarfs?
Double Degenerate Scenario (DD).
Image Credit: NASA/Tod Strohmayer (GSFC)/
Dana Berry (Chandra X-Ray Observatory)

Our Strategy: Finding Legacies of Supernova
Explosions in Supernova Remnants～450yrs later

Tycho Supernova Remnant in the Milky Way
The Painting was done by Camille Flammarion (1880)

Tycho Supernova in 1572

Image Credit: MPIA/Spitzer Space Telescope/
Chandra X-Ray Observatory /Calar Alto 3.5m TelescopeAn Analogy: From T-REX Fossil to T-REX?
?

From Amazon Free-download.

The Tyrannosaurus rex fossil known as Stan is displayed in a gallery atChristie’s auction house in New York City on September 17, 2020.
PHOTOGRAPH BY SPENCER PLATT, GETTY IMAGES

Without any doubt, Fossils of Dinosaurs contain lots of
information on Dinosaurs.
The problem is how accurately we understandDinosaurs from their fossils.

By Chris Packham (2017)

Our Strong Points• Only our group succeeded to perform 3-dimensional simulations ofsupernova remnants from supernova phase.
• Only our group succeeded to solve rate equations of atomic processes
for non-thermal ionizations for 3-dimensional simulations of supernova
remnants from supernova phase.
• Our group is sustained by long-lasting, international collaborations.
We adopt a co-moving
grid system for
Hydro simulations.

～450yrs later～13,000km

From HP of Prof. David Taylor～2×10/@ km.

A Type Ia Supernova Simulation (SD Model)

Friedrich Röpke

Ivo Seitenzhal

Florian Lach

From a Supernova to a Supernova Remnant
x=0 slice (Density)

Iso-surfaces of density

Gilles Ferrand

Evolution: 10 to 450 yrs

Shiu-Hang Lee(Herman)

Spherical harmonics expansion of the wavefronts
contact discontinuity (CD) from 1 yr to 500 yr
From Supernova
To Supernova Remnant

Gilles Ferrand

From a Simple
Spherically Symmetric
Initial Condition

Large Scale

Small ScaleRayleigh-Taylor from the SN and SNR phases
contact discontinuity (CD) at 500 yr
From Supernova
To Supernova Remnant
SN modesSNR RTI

Gilles Ferrand

From a Simple
Spherically Symmetric
Initial Condition

Large Scale

Small Scale
SNR RTI

Solving Rate Equations for Non-Equilibrium
Ionization States
Shocked particles in ejecta(N particle = 100,000 in shown example)

Color = neColor = Tet = 20 to 450 yrs
10 yrs per frame

Shiu-Hang Lee(Herman)
Lee et al. (2023)
in prep.

21

ionT=logt = 20 to 450 yrs
10 yrs per frame

Ion temperature per species
̶> thermal broadening of lines

Coulomb heatingeTcolor = nenISM = 1.2 cm-3

Lee et al. (2023)
in prep.
22<Tion> vs Telog

From DD-Type Ia Supernova to Supernova Remnant
500 yrsc.f. Type Ia SNR 0509-68.7
in Large Magellanic Cloud.
X-ray Image.

Ataru Tanikawa

Gilles Ferrand

Asymmetries of Supernova Explosion
are imprinted in Supernova Remnantsin Large Angular Scale.

Credit: NASA/CXC/SAO

Massive Stars also Explode as Supernovae
Massive Stars ≡ Stars with mass of (10–25) M, .

Neutrinos

NSImage Credit: Penn State Astronomy& Astrophysics

Iron Core Collapses and Neutron Star (NS) is formed at the Center.
The stiff NS makes an out-going shock wave and neutrinos from the NS
heat the shock wave, which results in a supernova (e.g. Bethe & Wilson 1985).

Theory of Astrophysics!

The Observational Proof：Detections of Supernova Neutrinos

The 11 events of neutrinos fromSN1987A, detected by Kamiokande.

SN1987A happened in Large
Sanduleak -69°202, theMagellanic Clouds on 23 Feb. 1987.
Progenitor Star of SN1987A.
The visible SN by naked eyes, about
Blue-Super Giant.
350yrs after the last one (Cassiopeia A).
～20 M! .

Masatoshi KoshibaNobel Prize in Physics 2002
for the detection ofcosmic neutrinos.

The Iron Emission Lines from SN1987A Changed My Life.

Blue Shift Side:
Toward Us(North Side).

Red Shift Side:
Away from Us(South Side).

From this line profile, we concluded in
1997-2000 that・ SN1987A was a Bi-Polar like explosion.
・ Explosion was stronger in Red Shift Sideand weaker in Blue Shift Side.
・ The Neutron Star of SN1987A should
be moving toward Blue Shift Side.

Haas et al. 1990

S. Nagataki

K. SatoM. Hashimoto

S. Yamada

I got my Ph.D. degree in 1998, and I became an assistant professor in 2001.
Thesis Title: “Effects of Jet-Like Explosions in Collapse-Driven Supernovae”

Bi-Polar Explosion was Confirmed.
Image of 87A by
Hubble Space Telescope
Figure from Larsson et al.
(2019).
Supernova Ejecta
Ring was formed
BEFORE the Supernova.
Our 1st paper wasSubmitted (21 Feb. 1997)
and Accepted (21 Apr. 1997)
Here.
23rd Feb. 1997 was the 10th
Anniversary of SN1987A.
Last week, SN1987A became
36 yrs old.

Evidence of Stronger Explosion in Red-Shift Side (South Side)
NorthSouth

Image of [Fe I] 1.443μm line by JWST.
Larsson et al. (2023)

The James Webb Space Telescope( JWST, 2021- )Evidence of the NS running toward the North?

Heated by the NS?

Explosion
CenterRadio Image of SN1987A in 2015 by ALMA (Cigan et al. 2019), overlapped with
Optical Image in 2014 by Hubble Space Telescope (Fransson et al. 2015)

Our Recent SN1987A Simulation from Progenitor Star

H. Umeda

From SN to SNR
Simulation.

T. Yoshida

M. OnoS. Orlando

We found that Bi-polar like explosions of a binary
Progenitor star model explain many observations of 87A.
Distribution of Iron for different progenitor models.

Our SN-SNR Project solved the Long-Lasting Mystery of Cas A.
Blue: 44Ti
Green: Si/Mg
Red: FeSN Phase

A. Wongwathanarat S. Orlando
Sato et al. 2021

Image Credit: Chandra: NASA/CXC/RIKEN/T. Sato et al.;NuSTAR: NASA/NuSTAR; Hubble: NASA/STScI

Fe-richS/O-rich

Milisavljevic & Fesen 2013

Cassiopeia A, the Youngest CC-SNR in the Milky Way (～350 yrs old).

SNR Phase

T. JankaWe proved that the Iron Blob was ejected byNeutrino-Driven Winds from the NSToshiki Sato

By the detailed analysis, we found
Not only Fe, but also Ti and Cr.
Our study was introduced at theCover page of Nature Vol. 592, Apr.2021

H. Umeda

Takashi Yoshida

K. Maeda

J. Hughes

Gravitational Waves may Shed Light on the Structure of Neutron Stars

Y. Huang

L. Baiotti

T. KojoT. Hatsuda

Physics!
～(20-25)km?

Image Credit:
NASA’s Goddard Space Flight Center/ Conceptual Image Lab

General Relativistic Hydro Simulation and Resulting GWs

K. Takami

Yamamoto, Tachibana, Baym, Hatsuda (2006)

H. TogashiThe Origin of Life is Supernova Explosions

Contribution of Type Ia SNe ～10%
Contribution of CC-SNe ～ 90%

Figure from Tsujimoto et al. 1995

Composition of the Earth:
O ～32.4%
Fe～28.2%
Si ～17.2%
Mg～15.9%
Ni ～ 1.6%
Ca～ 1.6%
Al ～ 1.5%
in mass (Wt%).
Allègre et al. 1995

List of Our Group’s 14 Papers in This Talk
Type Ia Supernova Remnants:
・ Ferrand, G., Tanikawa, A., Warren, D.C., Nagataki, S., Safi-Harb, S., Decourchelle, A. The Astrophysical Journal, 930, id.92 (2022).
・ Ferrand, G., Warren, D.C., Ono, M., Nagataki, S., Röpke, F. K., Seitenzahl, I. R., Lach, F., Iwasaki, H., Sato, T., The AstrophysicalJournal, 906, id.93 (2021).
・ Ferrand, G., Warren, D., Ono, M., Nagataki, S., Röpke, F. K., Seitenzahl, I. R., The Astrophysical Journal, Volume 877, id. 136 (2019).
・ Lee, S.H. et al. in prep. (2023).

Core Collapse Supernova Remnants:
・ Orlando, S.; Wongwathanarat, A.; Janka, H. -T.; Miceli, M.; Nagataki, S.; Ono, M.; Bocchino, F.; Vink, J.; Milisavljevic, D.; Patnaude, D.
J.; Peres, G., Astronomy & Astrophysics, Volume 666, id.A2, 19 pp. (2022).
・ Sato, Toshiki; Maeda, Keiichi; Nagataki, Shigehiro; Yoshida, Takashi; Grefenstette, Brian; Williams, Brian J.; Umeda, Hideyuki; Ono,Masaomi; Hughes, John P., Nature, Volume 592, Issue 7855, p.537-540 (2021).
・ Orlando, S.; Wongwathanarat, A.; Janka, H. -T.; Miceli, M.; Ono, M.; Nagataki, S.; Bocchino, F.; Peres, G., Astronomy & Astrophysics,
Volume 645, id.A66, 32 pp. (2021).
・ Orlando, S.; Ono, M.; Nagataki, S.; Miceli, M.; Umeda, H.; Ferrand, G.; Bocchino, F.; Petruk, O.; Peres, G.; Takahashi, K.; Yoshida, T.,
Astronomy & Astrophysics, Volume 636, id.A22, 19 pp. (2020).
・ Ono, M., Nagataki, S., Ferrand, G., Takahashi, K., Umeda, H., Yoshida, T., Orlando, S., Miceli, M., The Astrophysical Journal, Volume888, Issue 2, id.111, 40 pp. (2020).
・ Orlando, S., Miceli, M., Petruk, O., Ono, M., Nagataki, S., Aloy, M. A., Mimica, P., Lee, S. H., Bocchino, F., Peres, G., Guarrasi, M.,
Astronomy & Astrophysics, Volume 622, id.A73, 15 pp. (2019).
・ Nagataki, S., The Astrophysical Journal Supplement Series, Volume 127, Issue 1, pp. 141-157 (2000).
・ Nagataki, S., Hashimoto, M., Sato, K., Yamada, S., The Astrophysical Journal, Volume 486, Issue 2, pp. 1026-1035 (1997).
・ Lee, S.H. et al. in prep. (2023).

Neutron Star Mergers and Gravitational Waves:・Huang, Yong-Jia; Baiotti, Luca; Kojo, Toru; Takami, Kentaro; Sotani, Hajime; Togashi, Hajime; Hatsuda, Tetsuo; Nagataki, Shigehiro; Fan,Yi-Zhong, Physical Review Letters, Volume 129, Issue 18, article id.181101 (2022).

Thank You Very Much.

Friedrich Röpke

Ivo Seitenzahl

Florian Lach

Gilles Ferrand

Shigehiro Nagataki

Shiu-Hang Lee(Herman)

My Lecture on
Stellar Astrophysics
at OIST will start in Sep. 2023.

Ataru Tanikawa

Masaomi Ono

Katsuhiko Sato Masaaki Hashimoto Shoichi Yamada Hideyuki Umeda Takashi Yoshida Keiichi Maeda Toshiki Sato Annop

Wongwathanarat

Salvatore Orlando

Thomas Janka John Hughes

KentaroYongjia Huang Luca Baiotti Toru Kojo Tetsuo Hatsuda TakamiHajimeTogashi