stellar neutrinos 2020 - arizona state...

1) Neutrino astronomy 2) Neutrino production in stars 3) MESA 4) Neutrino HR diagram 5) Probing the presupernova isotopic evolution 6) Identifying the presupernova progenitor 7) Low mass stars count too

38 Slides

Roadmap

Bob King, Sky & Telescope, 22Dec2019

Over the next decade, neutrino astronomy will probe the rich astrophysics of neutrino production in the sky.

Energy (keV)

Eve

nts

per

day

× 1

00

t ×

Nh

10–3

10–2

10–1

1

10 14C210Po210Bi85KrTotal t: P = 0. 7

11CPile-upExternal background

pp

7Be

CNO pep 8B

Nh

100 200 300 400 500 600 700 800 900

500 1,000 1,500 2,000 2,500

40

30

20

10

00 2 4

time (s)

KamiokandeIMBBaksan

ener

gy (M

eV)

6 8 10 12

Borexino Collaboration

IceCube Collaboration

In addition to the Sun, supernova 1987A,

and blazar TXS 0506+056,

XENON dark matter projectJUNO aims to begin taking data in 2020.

Super-K with Gadolinium Test Facility

P

N

e+ a-ray

Gadolinium

Original detectable signal New signal

i

Super-Kamiokande with Gadolinium, Jiangmen Underground Neutrino Observatory, XENON and other experiments usher in a new generation of detectors designed to open new avenues for potentially observing currently undetected neutrinos.

ABSTRACT

Supernova detection is a major objective of the Super-Kamiokande (SK) experiment. In the nextstage of SK (SK-Gd), gadolinium (Gd) sulfate will be added to the detector, which will improvethe ability of the detector to identify neutrons. A core-collapse supernova will be preceded by anincreasing flux of neutrinos and anti-neutrinos, from thermal and weak nuclear processes in the star,over a timescale of hours; some of which may be detected at SK-Gd. This could provide an earlywarning of an imminent core-collapse supernova, hours earlier than the detection of the neutrinosfrom core collapse. Electron anti-neutrino detection will rely on inverse beta decay events below theusual analysis energy threshold of SK, so Gd loading is vital to reduce backgrounds while maximisingdetection e!ciency. Assuming normal neutrino mass ordering, more than 200 events could be detectedin the final 12 hours before core collapse for a 15-25 solar mass star at around 200 pc, which isrepresentative of the nearest red supergiant to Earth, !-Ori (Betelgeuse). At a statistical false alarmrate of 1 per century, detection could be up to 10 hours before core collapse, and a pre-supernovastar could be detected by SK-Gd up to 600 pc away. A pre-supernova alert could be provided to theastrophysics community following gadolinium loading.

Sensitivity of Super-Kamiokande with Gadolinium

to Low Energy Anti-neutrinos from Pre-supernova Emission

C. Simpson et al, The Super-Kamiokande Collaboration

ApJ, Nov 2019

Celestial Equator b=0à

0.6 kpc 0.4 kpc

0.2 kpc

O,B,A K M Name (M!, kpc)

Spica (11,0.08)

12Peg(6,0.42)

_�Cyg(19,0.80)

5 Lac(5,0.51)

V424 Lac (7,0.63)

HR 8248(6,0.75)

HR 861(9,0.64)

V809 Cas (8,0.73)

HR 3692 (12,0.65)

145 CMa (8,0.70) VV Cep (11,0.59)

V381 Cep (12,0.63)

S Mon A (29,0.28) CE Tauri (14,0.33) S Mon B (21,0.28)

q Car (7,0.23) w Car (8,0.29)

NS Pup (10,0.32)

c�Oph(20,0.11) _�Lupi (10,0.14)

h�Vel(7,0.17)

Antares(11,0.17)

+x

Vernal Equinox_= 0 hr

¡�Peg(12,0.21)

c�Cep(10,0.26)

e�Del(6,0.63)

j�Cyg(8,0.28)

_�Ori(12,0.22)

`�Ori(21,0.26) a2 Vel

(9.0, 0.34)

k1 CMa (8,0.39)

m CMa(12,0.51)

Mukhopadhyay et al 2020

Let’s explore recent theoretical results that provide

New targets for current, forthcoming, and future generations of neutrino detectors.

New estimates of the stellar neutrino background signal.

New opportunities for nuclear experiments that can make sizable differences in stellar evolution.

Neutrino Production in Stars

Stars radiate energy by releasing photons from the stellar surface and neutrinos from the stellar interior.

�⌫ ' (E⌫/mec2)2 · 10�44 cm2

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�� =8⇡

3

✓↵~cmec2

◆2

' 10�24 cm2

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�⌫ =mu

⇢ · �⌫

��' 3 · 1019cm ' 10pc ' 4 · 109R�

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⌧⌫ ' R�/c ' 2 s

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Weak reactions produce neutrinos by thermal processes

Log10 (thermal neutrino loss rate) erg g-1 s-1 for X(12C)=1

-10 -5 0 5 10 15Log

10 Density (g/cm 3)

7

7.5

8

8.5

9

9.5

10Lo

g 10 T

emp

erat

ure

(K)

-5

0

5

10

15

20

25

30

35

Pair neutrino

Photoneutrino

Plasmon

Bremsstrahlung

Reco

¡nuc = ¡ie+ + e- A�i��i

e-continuum A�e-bound + i��i

aplasmon A�i��i

e- + a A�e- + i��i

e- + ZA A�e- + ZA + i��i

Weak reactions produce neutrinos from β-processes

De-excitation: AZZ0

��! AZ + ⌫ + ⌫̄e

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Electron captures:

p+ e�W±��! n+ ⌫e

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AZ + e�W±��! A(Z � 1) + ⌫e

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Positron captures: AZ + e+W±��! A(Z + 1) + ⌫̄e

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n+ e+W±��! p+ ⌫̄e

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Electron emission (β- decay): AZW±��! A(Z + 1) + e� + ⌫̄e

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nW±��! p+ e� + ⌫̄e

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Positron emission (β+ decay): AZW±��! A(Z � 1) + e+ + ⌫e

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pW±��! n+ e+ + ⌫e

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A Stellar Evolution Instrument

The MESA source code is a set of software modules for stellar astrophysics that can be used on their own, or combined to solve the coupled equations governing 1D stellar evolution with an implicit finite volume scheme.

PTLR

1H3He4He12C14N16O

20Ne24Mg

Variables

Equ

atio

ns fo

r cel

l k

cell k-1 cell k cell k+1

d(structk)d(structk-1)

d(chemk)d(chemk-1)

d(chemk)d(chemk+1)

d(chemk)d(chemk)

d(chemk)d(structk)

d(structk)d(structk+1)

d(structk)d(structk)

d(structk)d(chemk)

South 3DFLĆFOcean

South AtlanticOcean

North AtlanticOcean

North 3DFLĆFOcean

IndianOcean

MESA : Community of ~1000, Jan 2020

Josiah Schwab Evan Bauer

Rob Farmer

Warrick Ball

Anne Thoul

Bill Wolf

Pablo Marchant

Matteo CantielloRich Townsend Bill Paxton Lars BildstenFrank TimmesAaron Dotter

Radek Smolec

Adam Jermyn Meridith Joyce

Citations: 4,279

Citations to articlesthat cite MESA: 80,859

Larger Science Community

MESA

ImpactRadius Ā20

Cita

tions

0

275

550

825

1100

2011 2012 2013 2014 2015 2016 2017 2018 2019 2020

MESA I - Top 5 in 2011MESA II - Top 10 in 2013MESA III - Top 10 in 2015MESA IV - Top 15 in 2018MESA V - Top 25 in 2019

Data from SAO/NASA ADS

Pulsations:

Stars:

Pulsations:

Adipls

MESA

Support:

Support:

Cyberhub:

NuGrid

Nuclear:

StarLibNuclear:

AZURE

3D hydro:

Athena++

3D hydro:

FLASH

3D hydro:

Dedalus

MAESTRO

3D hydro:

PPMStar

3D hydro:

Phantom

Opacity:

Opacity:

3D hydro:

ASTROBEAROP

OPLIB

3D hydro:

Changa

3D hydro:

ENZO

GAMMA

PyMESA

VMESA

MESA-Docker

Support:

GCE:

Ports:

SYGMAYields:

YTVisualization:

emceeAnalysis:

OMEGA

GCE:

Support:

HYPATIAStars:

AstropyAstro:Stars:

JINABase

3D hydro:

3D hydro:

Isochrones:

GYRE

N-Body:Amuse

Spectra:

Spectra:Chemistry: Chemistry:

CLOUDY

CMFGENGrackle KROME

StarCrash

Education:

MESA-Web

Support:

NuDocker

Development:

MESA-Test

Stars:

Dstar

Nuclear:

JINAReaclib

Radiation:

STELLA

Pulsations:

RSP

Nuclear:

WeakLib

MI T

NSCL FRIB CASPAR SECAR St. George Z-Pinch Diamond Anvil

Laboratory Astrophysics

Telescopes

1D 3DMESA2HYDRO

GRMHD:

Einstein Toolkit

ASAS-SN ZTFLIGO Hubble NuSTARVRO LCOGaia SK-GdSDSS JWST TESS

Neutrino HR diagram

Solar Neutrino Fluxes

Component AGSS09 GS98 Observeda

!pp 6.01 5.98 6.05(1+0.003!0.011)

!Be 4.71 4.95 4.82(1+0.05!0.04)

!B 4.62 5.09 5.00(1 ± 0.03)

!N 2.25 2.91 ! 6.7

!O 1.67 2.21 ! 3.2

aNeutrino observations from the Borexino Collabo-ration (Bellini et al. 2011) as presented in Haxtonet al. (2013) and Villante et al. (2014). The scalesfor neutrino fluxes ! (in cm-2 s-1) are: 1010 (pp);109 (Be); 106 (B); 108 (N); and 108 (O).

Farag et al 2020

Lν,⊙ = 0.024 · Lγ,⊙ = 9.18 × 1031 erg/s

A MESA standard solar model

Farag et al 2020

The ~110 year old classic HR Diagram.

One doesn’t mess with a classic …

… but what if …

Farag et al 2020

A neutrino HR Diagram!

Farag et al 2020

When do photons or neutrinos dominate?

Neutrinos tend to dominate at the end of star’s life.

Farag et al 2020

When do thermal neutrino or β-processes dominate?

β-processes tend to dominate whenever H or He burns.

Probing the evolution of pre-supernova models

Si Burning

early warning,SN direction,progenitor physics

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Mantle Contraction Cooling

Core Cooling }}

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HTXDWLRQ�RI�VWDWH��energy loss rates, PNS radius, GLIIXVLRQ�WLPH��BSM physics

i<Sphere Recession

16�YV��%+�IRUPDWLRQ��WUDQVSDUHQF\�WLPH��integrated losses, BSM physics

Fallback

1053

1052

1051

1050

1049

1048

1047

��2 0

7LPHSRVW�ERXQFH (s)

10�� 100 101 102 103

3UH�61 Main Signal /DWH�7LPH

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Following Li, Roberts & Beacom,

2020

The march to core-collapse.

1046

1048

1050

1052

1054

L! ! N

(s!

1)

O core

O shell

2nd O shell

Si core

Si shell

9.0

9.2

9.4

9.6

9.8

10.0

cLog

(T/K

)

O burning

Si burning

10!410!2100102104

!CC (hr)

6.0 6.5 7.0 7.5 8.0 8.5 9.0 9.5 10.0 10.5

Log(!c/g cm!3)

"x/"̄x pair"e/"̄e pair

"̄e #"e #

15M 15M

Patton et al 2017

β-process rates that matter. Isotopes listed for neutrinos are mainly electron captures, those for antineutrinos are mainly β- decay. We encourage new experiments and theory!

0.06 s

ie

ie

53Fe - 17%55Fe - 15%55Co - 14%54Mn - 10%57Ni - 4%

56Mn - 43%52V - 11%57Mn - 8%62Co - 7%55Cr - 7%

p - 23%53Cr - 7%51V - 5%55Mn - 5%55Fe - 4%

58Mn - 15%54V - 9%63Co - 7%55Cr - 6%59Mn - 6%

46 s

0.5 hr

1.0 hr

2.0 hr

Si burning

O burning

15 M!

6.0

9.0

9.2

9.4

9.6

9.8

10.0

Log (lc / g cm-3)

Log

(Tc

/ g

cm-3

)

7.0 8.0

Ei�ă 2 Mev

9.0 10.0

0.1 hr

ie

ie

Patton et al 2017

Patton et al 2017

Pre-supernova fluxes at 1 kpc : as strong as solar neutrinos, larger than background geo or reactor neutrinos.

2 hr

2 hr

0.4 s

Energy (Mev)

solar ireactor i

geo i

30 M!, ie , NH, 1 kpc

Flu

x at

Ear

th (M

ev-1

s-1

cm

-2)

Energy (Mev)1.0 1.010.0 10.0

104

106

108

1010

0.4 s0.0 s

0.0 s

30 M!, ie , NH, 1 kpc

“A prime example is the red supergiant Betelgeuse (α Orionis) … We find that for D=200 pc, a presupernova neutrino signal would be practically background-free — in energy windows that are realistic for detection — for several hours, and the window of observability can extend up to ∼10 hr.”

Patton et al 2017

Simpson et al 2019

“A presupernova alert could be provided to the gravitational wave and electromagnetic communities …”

Identifying the Progenitor

n

ea

_ei p

X(i)pn

e+


In a liquid scintillator detector:

0

20

40

60

80

100

120

140

0

10

20

30

40

50

60

N

``

0 100 200 300 400 500

0 100 200 300 400 500

LS

68% C.L.

68% C.L.

90% C.L.

90% C.L.

LS-Li

310þ

310þ

310þ

310þ_

_

_

_

Standard liquid scintillators could localize the pre-supernova to ~ 70° after~100 detections.

Enhanced liquid scintillators could localize the pre-supernova to ~ 15° after ~100 detections.


Antares 0.17 pc 15 M!

t-minus 4 hr

75à 60à

45à

30à

15à

-15à

-30à

-45à

-60à -75à

0à

RA

Dec

210 180 150 120 90 60 30 0 330 300

Galactic PlaneLS, 65% CL

LS, 95% CL

LS-Li, 65% CL

LS-Li, 95% CL

D Ă 0.25 kpc0.25 <D Ă 0.6 kpc0.6 <D Ă 1.0 kpc

Antares 0.17 pc 15 M! 75à 60à

45à

30à

15à

-15à

-30à

-45à

-60à -75à

0à

RA

Dec

180 150 120 90 60 30 0 330 300

t-minus 1 hr

Galactic PlaneLS, 65% CLLS, 95% CL

LS-Li, 65% CL

LS-Li, 95% CL

Antares 0.17 pc 15 M! 75à 60à

45à

30à

15à

-15à

-30à

-45à

-60à -75à

0à

RA

180 150 120 90 60 30 0 330 300 Dec

LS-Li, 95% CL

t-minus 2 min

Galactic PlaneLS, 65% CL

LS, 95% CL

LS-Li, 65% CL


Probing the evolution of low mass models

The He-burning driven thermal pulses reach Lν ≃ 109 Lν,⊙ mostly from the 18F(,e+νe)18O reaction .

flux Φν,Thermal Pulse ≃ 1.7x107 (10 pc/d)2 cm-2 s-1 timescale ≃ 0.1 year average νe energy ≃ 0.3 MeV

Farag et al 2020

flux Φν,He flash ≃ 170 (10 pc/d)2 cm-2 s-1 timescale ≃ 3 days average νe energy ≃ 0.3 MeV

The He-flash reach Lν ≃ 104 Lν,⊙ mostly from the same reaction .

3

GL 54.1

GL 358

Oort Cloud

Barnard StarAC+79 3888

Sirius

GL693

GL806A

GL682

Ross 128

Lalande21185

_-Cen A/B + Proxima

2

1

0-100 -50 50 100

Time (kyr)

Hel

ioce

ntr

ic D

ista

nce

(pc)

0

No good nearby targets for detections of the He-flash or thermal pulse.

After García-Sánchez et al 1999

Time for a Neutrino Cocktail

stellar neutrinos 2020 - arizona state...

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