A new aesthetic proposal for “Men at arms” by Donato Bramante
AuGenesis Joseph Bramante TEVPA2017 · AuGenesis_Joseph_Bramante_TEVPA2017 Created Date: 8/7/2017...
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Tim Linden OSU Fatemeh Elahi IPM Nirmal Raj Notre Dame Masha Baryakhtar Perimeter Shirley Weishi Li SLAC Yu-Dai Tsai Cornell, PI
Transcript of AuGenesis Joseph Bramante TEVPA2017 · AuGenesis_Joseph_Bramante_TEVPA2017 Created Date: 8/7/2017...
Tim LindenOSU
FatemehElahiIPM
NirmalRajNotre Dame
MashaBaryakhtarPerimeter
Shirley Weishi LiSLAC
Yu-Dai TsaiCornell, PI
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DILUTE
DILUTION FACTOR ζSee also
Allahverdi Dutta Sinha '11 Kane Shao Watson ’11
Davoudiasl Hooper McDermott ’15 Berlin Hooper Krnjaic '16
σn (cm2)
mx (GeV)10 1000 105 107
10-48
10-46
10-44
10-42
10-40
10-38
simplest case: let mx = mv
x xwimp
ζ = 1 10 -2 10 -4 10 -6 10 -8 10 -10
σn (cm2)
mx (GeV)10 1000 105 107
10-48
10-46
10-44
10-42
10-40
10-38
simplest case: let mx = mv
x xwimp, αw
ζ = 1 10 -2 10 -4 10 -6 10 -8 10 -10
σn (cm2)
mx (GeV)10 1000 105 107
10-48
10-46
10-44
10-42
10-40
10-38
simplest case: let mx = mv
x xstrong
ζ = 1 10 -2 10 -4 10 -6 10 -8 10 -10
σn (cm2)
mx (GeV)10 1000 105 107
10-48
10-46
10-44
10-42
10-40
10-38
simplest case: let mx = mv
x xstrong
dilution bound for high scale
baryogenesis, ζ>10-10
ζ = 1 10 -2 10 -4 10 -6 10 -8 10 -10
σn (cm2)
mx (GeV)10 1000 105 107
10-48
10-46
10-44
10-42
10-40
10-38
simplest case: let mx = mv
x xstrong
see Nirmal Raj tomorrow 3pm to find dilute wimps with neutron stars
2 3 4 5 6 7 8 9-14
-12
-10
-8
-6
-4
Log[mDM/GeV]
Log[η D
M
]
ζ = 1
initi
al
ζ = 10 -2
ζ = 10 -10
ζ = 10 -4
ζ = 10 -6
ζ = 10 -8
αDM = 0.3 αDM = 0.05
2 3 4 5 6 7 8 9-14
-12
-10
-8
-6
-4
Log[mDM/GeV]
Log[η D
M
]
ζ = 1
initi
al
ζ = 10 -2
ζ = 10 -10
ζ = 10 -4
ζ = 10 -6
ζ = 10 -8
αDM = 0.3 αDM = 0.05
Example: PeV sector⌘(1)B
⌘(2)DM
'✓
M
m�B
◆ 13
' 104✓
M
MPl
◆ 13✓1 PeV
m�B
◆ 13
Gold from Heavy Asymmetric DM and Neutron Star Implosions
1. Heavy asymmetric dark matter implodes neutron stars by collecting inside, and forming black holes at
their cores.
JB Linden 2016JB Linden Tsai 2017
Gold from Heavy Asymmetric DM and Neutron Star Implosions
1. Heavy asymmetric dark matter implodes neutron stars by collecting inside, and forming black holes at
their cores.
JB Linden Tsai 2017
see Yu-Dai Tsai tomorrow 245pm to find HADWIMPS with neutron stars,
gravity waves, kilonovae, and frbs JB Linden 2016
Gold from Heavy Asymmetric DM and Neutron Star Implosions
1. Heavy asymmetric dark matter implodes neutron stars by collecting inside, and forming black holes at
their cores.
2. Imploding neutron stars eject neutron star fluid that forms heavy r-process elements (gold).
3. DM-induced neutron star implosions can explain why r-process elements are in just one of ten dwarf galaxies.
JB Linden 2016JB Linden Tsai 2017
-R-process elements: heavy elements with atomic masses around ~80, ~130, ~195-Formed in an as-yet-undetermined astrophysical sites rich in neutrons
Reifarth et al. 2014 s-process,formed in typical stars
r-process nuclei,formed where?
Possible r-process sites — total 104 M⨀ produced in Milky Way
-Neutrons ejected by neutrino wind during core collapse supernovae (frequent, ~1/100 years)
-Merging neutron star binaries, tidal forces expel dense neutron star fluid (rare, ~1/104 years)
-Neutrons ejected by neutrino wind during core collapse supernovae (frequent, ~1/100 years)
-Merging neutron star binaries, tidal forces expel dense neutron star fluid (rare, ~1/104 years) -Neutron star slurped into a black hole made of heavy asymmetric dark matter at its core.
In each case, neutron rich fluid beta decays, forms heavy neutron-rich elements.
implosiontidally expelssomeneutron fluid
Possible r-process sites — total 104 M⨀ produced in Milky Way
np
Wnnnnnnnnnnnn
nnnnnn
nnnnnn … Gold,Uranium, Europium, Barium…
R-process in Ultra Faint Dwarf Galaxies
-Alexander Ji, grad student — "go look for r-process elements in ultra-faint dwarfs"
-Ultra faint dwarfs are star-poor dwarf galaxies formed in a billion year burst ~10 billion years ago
R-process in Ultra Faint Dwarf Galaxies
-Alexander Ji, grad student — "go look for r-process elements in ultra-faint dwarfs"
-Ultra faint dwarfs are star-poor dwarf galaxies formed in a billion year burst ~10 billion years ago -Found just one with high r-process abundance — low r-process abundance expected in all ultra faint dwarfs
One UFD with r-process, and 9 without, implies rare r-process events.
many CCSN few NS mergers few implosions
Ji et al. 2016
Plot of r-process in dwarfs — grey points are MW stars ➔ [X/Y] is log(X/Y) abundance.
➔ Ba, Eu are r-process elements, [Fe/H] grows with age
Unexpectedly high r-process abundance in Reticulum II -indicates r-process from rare event
Reticulum IIhigh r-process abundance
Other dwarfs,low r-process abundance
Plot of r-process in dwarfs — grey points are MW stars ➔ [X/Y] is log(X/Y) abundance.
➔ Ba, Eu are r-process elements, [Fe/H] grows with age
**Neutron stars kicked at birth ~100 km/s.
**This kicks NS binary system to ~50 km/s.
**Merging neutron stars are ejected from dwarf spheroidals
—Reticulum II escape velocity <10 km/s.
NS mergers kicked out of Reticulum II
UFD escape velocity
Probability of one merger for 10 UFDs
JB, Linden '16
NS mergers kicked out of Reticulum II
**Neutron stars kicked at birth ~100 km/s.
**This kicks NS binary system to ~50 km/s.
**Merging neutron stars are ejected from dwarf spheroidals
—Reticulum II escape velocity <10 km/s.
UFD r-process rates
104 105 106 10710-4
0.001
0.01
0.1
1
10
100
Total Stellar Mass of UFDs (M⊙)
R-P
roce
ss E
vent
s in
500
Myr
CCSNe
DM-induced NS implosions, vesc=10 km/s
NS merger, vesc=10 km/sNS mergers, vesc=100 km/s (u
nrealistic)
Probability of one event
0.36
0.09
0.01
0.001
10-3.3
10-41
10-4
Too many
Just right
Too few
-Tuned towards atomic stability & production in supernovae-Shift mass or couplings ⇒ supernovae disrupted
⇒ destabilize nuclei
Cosmologically Stable Particles + Bosons
All cosmologically stable matter tuned for heavy element production.
DarkMatter
Variation on Atomic Principle
-Tuned towards atomic stability & production in supernovae-Shift mass or couplings ⇒ supernovae disrupted
⇒ destabilize nuclei
Cosmologically Stable Particles + Bosons
