Explosive Dark Matter Production of Heavy Elements in Compact Stars - - PowerPoint PPT Presentation

Explosive Dark Matter Production of Heavy Elements in Compact Stars

Joseph Bramante Queen’s University McDonald Institute Perimeter Institute Solvay Institute Dark Side of Black Holes Workshop

100 10-10 1010 1020 1030 1040 1050 1060 10-20 10-30 Strongly Interacting Massive Particles Axions Alps Hidden Photons Fuzzy Dark Matter

No Half- Integer Spin Zone

WIMPs Heavier WIMPs Primordial Black Holes Exotic Compact Objects a.k.a. Bound State Dark Matter

(can’t fit enough fermions into galaxies because of degeneracy pressure)

mx (GeV)

Mass of Smallest Galactic Halos

de Broglie length = size of dwarf galaxy

Dark Matter Models (We Know Very Little)

100 10-10 1010 1020 1030 1040 1050 1060 10-20 10-30 Strongly Interacting Massive Particles Axions Alps Hidden Photons Fuzzy Dark Matter

No Half- Integer Spin Zone

WIMPs

Compact Stars and Small BHs

Primordial Black Holes

Exotic Compact Objects a.k.a. Bound State Dark Matter

(can’t fit enough fermions into galaxies because of degeneracy pressure)

mx (GeV)

Mass of Smallest Galactic Halos

de Broglie length = size of dwarf galaxy

Dark Matter Models (We Know Very Little)

Superradiance

1989 Dark Matter forming Black Holes In compact stars Goldman and Nussinov

1989

Kouvaris, Tinyakov de Lavallaz, Fairbairn Kouvaris, Tinyakov

2011

Kouvaris, Tinyakov

Goldman and Nussinov 2012 2013 2014 2010 2015 2016 2017 2018

McDermott, Yu, Zurek Kouvaris, Tinyakov JB, Fukushima, Kumar Bell, Melatos, Petraki JB, Fukushima, Kumar, Stopnitzky Bertoni, Nelson, Reddy Kouvaris Kouvaris, Tinyakov, Tytgat JB, Linden, Tsai JB, Linden JB JB, Elahi JB, Linden JB, Delgado, Martin JB, Unwin Gresham, Zurek Autzen, Kouvaris Garani, Genolini, Hambye Guver Erkoca, Reno, Sarcevic Fuller, Ott Zheng, Sun, Chen

Dark Matter forming Black Holes In compact stars

1989

Kouvaris, Tinyakov de Lavallaz, Fairbairn Kouvaris, Tinyakov

2011

Kouvaris, Tinyakov

Goldman and Nussinov 2012 2013 2014 2010 2015 2016 2017 2018

McDermott, Yu, Zurek Kouvaris, Tinyakov JB, Fukushima, Kumar Bell, Melatos, Petraki JB, Fukushima, Kumar, Stopnitzky Bertoni, Nelson, Reddy Kouvaris Kouvaris, Tinyakov, Tytgat JB, Linden, Tsai JB, Linden JB JB, Elahi JB, Linden JB, Delgado, Martin JB, Unwin Gresham, Zurek Autzen, Kouvaris Garani, Genolini, Hambye Guver Erkoca, Reno, Sarcevic

Dark Matter forming Black Holes In Compact Stars

Compact Stars Collecting Dark Matter

Collect dark matter over a radius Reff = Rs vesc vx

Reff ~ 5000 km

Compact Stars Collecting Dark Matter

Collect dark matter over a radius Reff = Rs vesc vx Limit: saturation cross-section, total flux Total capture = (flux)(effective area)(fraction captured) σsat ∼ πR2

s

Nn

apture (0.3 GeV/cm3)vx Neutron Star: White Dwarf: ∼ 1012M/Gyr

∼ 1015M/Gyr

Dark Matter Imploding Neutron Stars

CX ∝ ρxσnx vx

= DM density × DM-nucleon cross section DM velocity capture rate vx velocity ρx density in MW halo

σnx

determines whether DM scatters, becomes grav bound DM pulled in by neutron star grav potential

• 1. DM captured

→~10-14 solar masses of dark matter in 10 billion years (near solar position)

• 1. DM captured
• 2. DM thermalizes

Harmonic oscillator potential

kBT ∼ Gρwdmxr2

th

Thermalization radius

rth rth ∼ 1 millimeter r PeV mx r Tns 105 K

Dark Matter Imploding Neutron Stars

• 1. DM captured
• 2. DM thermalizes

ρDM > ρns

M ferm

crit

' M 3

pl/m2 X

DM will collapse to a black hole if it

• 1. Self-gravitates
• 2. Exceeds its own degeneracy pressure
• 3. DM collapses

~10-14 solar masses for PeV mass DM

Dark Matter Imploding Neutron Stars

• 1. DM captured
• 2. DM thermalizes
• 4. BH consumes

neutron star

• 3. DM collapses

dMbh dt ≈ 4πρns(GMbh)2 v3

s

− 1 15360π(GMbh)2

Dark Matter Imploding Neutron Stars

• 1. DM captured
• 2. DM thermalizes
• 3. DM collapses
• 5. Form solar mass BH
• 4. BH consumes

neutron star

dMbh dt ≈ 4πρns(GMbh)2 v3

s

− 1 15360π(GMbh)2

Dark Matter Imploding Neutron Stars

Dark matter that implodes neutron stars

~GeV mass, asymmetric dark fermions — degeneracy pressure stabilizes up to a solar mass of dark matter.

X

Bosonic dark matter without repulsive self interactions — requires very small effective quartic (λ < 10-15).

✓

KeV-PeV

mx

(λ )

Heavy dark matter, fermionic or bosonic — fewer particles required for collapse.

✓

M bos

crit '

p λM 3

pl/m2 X

M ferm

crit

' M 3

pl/m2 X

PeV-EeV

BH for~10-14 solar masses

Bosonic DM Constraints JB, Kumar, et al. 2013

Estimate pulsar age measuring pulse period (P) and slowdown per pulse (Ṗ)

Pulsars Ṗ = P =

Estimate pulsar age measuring pulse period (P) and slowdown per pulse (Ṗ)

tNS = P 2 ˙ P

Pulsars Ṗ = P = =

divide by to find age

{

Using an old pulsar in the Milky Way the best sensitivity so far

105 106 107 108 109 1010 1011 1.×10-48 1.×10-47 1.×10-46 1.×10-45 1.×10-44 1.×10-43 1.×10-42

mx (GeV) σnx (cm2)

M W P u l s a r s

Xenon 1T

~10 NS Mergers

xenon SI ν floor

~100 NS Mergers

BH too small at formation, evaporates BH never forms

JB, Elahi 2015 J1738+0333, tNS~5 Gyr, binary WD companion with age of− 5 Gyr

More dark matter captured in the center of galaxies ➜so pulsar implosions occur there more rapidly.

r (kpc) ρDM (GeV/cm3)

0.01 0.1 1 10 1 10 100 1000

J Factor Einasto

2

NFW

1

Burkert

1/70

Dark Matter Halo Profiles

ρx (GeV/cm3)

DM capture in Milky Way:

Dark Matter Capture in MW

Cx ∝ ρx vx

0.001 0.010 0.100 1 10 1 10 100 1000 104

Radius (kpc)

IPeV, 10

• 4

8

, 10

• 1

5

) I G e V , 1 0-52 , ) I M e V , 1

• 4

7

, ) ITeV, 10

• 5

, 0)

HmX, snX [cm2], l) 10-4 0.001 0.01 0.1 1 10 105 106 107 108 109 1010

Radius from galactic center @kpcD Max Pulsar Age @yrsD mx = 1 P e V , σnX > 1 0-44 c m2

Dark Matter and Maximum Pulsar Age Curves

10-4 0.001 0.010 0.100 1 10 105 106 107 108 109 1010

[] []

• Milky Way’s 1-500 pc center surveyed

in the next decade by FAST, SKA.

ATNF Pulsar Catalogue Overlaid, ages from pulsar timing

mx = 3 P e V , σnx > 1 0-45 c m2

Dark Matter and Maximum Pulsar Age Curves

mx = 10 PeV, σnx > 10-44 cm2

The Missing Pulsar Problem

Many pulsars expected at galactic center Up to 1000 visible pulsars expected in central parsecs Only a few ~104 year old magnetars found so far 8 kpc

Sgr A*

e-

10 pc 8 kpc Milky Way Pulses broadened by electron scattering?

Dexter, O’Leary 1310.7022

Where are the galactic center pulsars?

• 1. Temporal pulse broadening scales with the

~fourth power of observation frequency

• 2. Magnetars (B~1014 Gauss) found in the

central parsec, allow for exact (multi-freq.) measurements of temporal pulse broadening from the galactic center

• 3. Based on these measurements, we should

have already seen up to ~100 millisecond period and ~100 "standard" period pulsars

e-

τ Δτ

e-

??

Where are the galactic center pulsars?

∆τ ∼ 1 s ✓Ghz ν ◆2

10-4 0.001 0.010 0.100 1 10 105 106 107 108 109 1010

[] []

• Milky Way’s 1-500 pc center surveyed

in the next decade by FAST, SKA.

ATNF Pulsar Catalogue Overlaid, ages from pulsar timing

mx = 3 P e V , σnx > 1 0-45 c m2

Dark Matter and Maximum Pulsar Age Curves

mx = 10 PeV, σnx > 10-44 cm2

Missing Pulsars

Missing Neutron Stars in our Galaxy Less Dark Matter More Dark Matter

Dark Matter?

Before observing a neutron star merger

• n August 18, 2017, we had only located

neutron stars in our own galaxy. With neutron star mergers we can hunt for dark matter in galaxies far far away.

Less Dark Matter More Dark Matter

We can now use the locations of neutron star mergers in other galaxies to hunt for neutron star imploding dark matter.

neutron star merger

Less Dark Matter More Dark Matter

neutron star merger

However:

• No neutron star age
• Have to seek DM with ingenuity or

statistics

R-process elements: heavy elements with peak abundances at atomic masses 80, 130, and 195, formed in a hot environment rich in free neutrons.

What makes gold? (elements near magic numbers) Recipe: lots of neutrons, very hot (109 K)

n p +

• 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)

Possible r-process sites

(total 104 M⨀ produced in Milky Way)

R-process elements from dark matter induced NS implosions

Neutron star implodes into a small black hole. Enough potential energy to eject up to ~msol fluid. "Tube of toothpaste" effect ejects neutron star fluid. Same timescale as NS-NS, BH-NS mergers ~ 1 ms.

RRoche ' 20 ✓ MBH 1010 M ◆1/3 ✓1014 g cm3 ρNS ◆1/3 m

JB, Linden 2016 See also: forthcoming numerical GR simulations from Perimeter colleagues

• 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

dark matter at its core. In each case, neutron rich fluid beta decays, forms heavy neutron-rich elements.

implosion tidally spurts neutron fluid

Possible r-process sites

(total 104 M⨀ produced in Milky Way)

n p W n n n n n n n n n n n n n n n n n n n n n n n n … Gold,Uranium, Europium, Barium…

• 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

dark matter at its core. In each case, neutron rich fluid beta decays, forms heavy neutron-rich elements.

implosion tidally spurts neutron fluid

Possible r-process sites

(total 104 M⨀ produced in Milky Way)

n p W n n n n n n n n n n n n n n n n n n n n n n n n … Gold,Uranium, Europium, Barium…

Self-Detecting Dark Matter (Ge, Xe, Ar are r-process elements)

R-process and DES Bounds

• n NS Implosion Kilonovae

10-6 10-5 10-4 0.001 0.010 0.100 0.5 1 5 10 50 100 500

1 09 M W P u l s a r s 1 B * , 1 C * D E S β = . 3

Mej [M⨀]

108 MW Pulsars 1B*

tc ρx/vx [Gyr GeV cm-3 / 200 km s-1]

5 Gyr Old Pulsar By Earth

R-process and DES Bounds

• n NS Implosion Kilonovae

10-6 10-5 10-4 0.001 0.010 0.100 0.5 1 5 10 50 100 500

1 09 M W P u l s a r s 1 B * , 1 C * D E S β = . 3

Mej [M⨀]

108 MW Pulsars 1B*

tc ρx/vx [Gyr GeV cm-3 / 200 km s-1]

5 Gyr Old Pulsar By Earth

ρx (GeV/cm3)

0.001 0.010 0.100 1 10 1 10 100 1000 104

Radius (kpc)

time until NS implosion varies with location

R-process and DES Bounds

• n NS Implosion Kilonovae

10-6 10-5 10-4 0.001 0.010 0.100 0.5 1 5 10 50 100 500

1 09 M W P u l s a r s 1 B * , 1 C * D E S β = . 3

Mej [M⨀]

108 MW Pulsars 1B*

tc ρx/vx [Gyr GeV cm-3 / 200 km s-1]

5 Gyr Old Pulsar By Earth

normalized time until NS implosion for GeV/cm3 (one Kouvaris)

ρx (GeV/cm3)

0.001 0.010 0.100 1 10 1 10 100 1000 104

Radius (kpc)

time until NS implosion varies with location

R-process and DES Bounds

• n NS Implosion Kilonovae

10-6 10-5 10-4 0.001 0.010 0.100 0.5 1 5 10 50 100 500

1 09 M W P u l s a r s 1 B * , 1 C * D E S β = . 3

Mej [M⨀]

108 MW Pulsars 1B*

tc ρx/vx [Gyr GeV cm-3 / 200 km s-1]

5 Gyr Old Pulsar By Earth

More than 104 r-process element production in Milky Way

DES all-sky kilonova search

(Too much gold bound!)

Black Mergers Quiet Kilonovae,

ρx (GeV/cm3)

0.001 0.010 0.100 1 10 1 10 100 1000 104

Radius (kpc)

Black merger: no kilonova accompanies collapsed NS mergers in galactic interior n p W Gravity Waves From LMBH mergers

JB, Linden, Tsai 2017

Black Mergers Quiet Kilonovae,

Black merger: no kilonova accompanies collapsed NS mergers in galactic interior n p W Gravity Waves From LMBH mergers 3 Kouvaris 15 Kouvaris No Kilonova

Black Mergers Quiet Kilonovae,

ρx (GeV/cm3)

0.001 0.010 0.100 1 10 1 10 100 1000 104

Radius (kpc)

Black merger: no kilonova accompanies collapsed NS mergers in galactic interior n p W Gravity Waves From LMBH mergers

Beacom-Hopkins ’06 Star Formation Sartore ’09 Final NS Distribution

3 Kouvaris 15 Kouvaris

Quiet Kilonovae: NS implosions create a less luminous kilonova, with no gravity wave signal n p W Gravity Waves From NS mergers

Quiet Kilonovae

No Observable GWaves

Quiet Kilonovae

Quiet Kilonovae: NS implosions create a less luminous kilonova, with no gravity wave signal n p W Gravity Waves From NS mergers No Observable GWaves

Wu, Barnes et al 2018 1808.10459

Modeled and Observed Kilonova Light Curves

Barnes, Kasen 2013

Neutron star fluid kilonovae last days and have luminosities that scale with ejected mass.

The SINS Survey — Finding Quiet Kilonovae In the Fornax Cluster

• 10 half nights every 3 days for 60 nights livetime
• Sensitivity to quiet kilonovae 0.2/yr per MWEG

NS Implosion Rate (could match Fast Radio Bursts)

JB, Linden, Tsai 2017

Rfrb ∼ 10−2 MWEG−1 yr−1 ✓ D 2 Gpc ◆−3

NS Implosions

• Incorporates

NS dynamics, birthrates in Milky Way, capture rate for position in galaxy

1 5 10 50 100 1.×10-4 5.×10-4 0.001 0.005 0.010 0.050

tc ρx/vx [Gyr GeV cm-3 / 200 km s-1]

5 Gyr Old Pulsar By Earth

Typical FRB rate

NS Implosions [MWEG-1 yr-1]

1 09 M W P u l s a r s 1 B * 1 08 M W P u l s a r s 1 B *

R-Process Donuts: Quiet kilonovae and standard NS merger kilonovae occur in donut shaped external regions of disc galaxies

n p W Gravity Waves From NS mergers

R-Process Donuts

Dark Matter Alters Neutron Star Merger Locations in Galaxies

Galactic Radius [kpc]

Merger Kilonova CDF

5 10 15 20 0.0 0.2 0.4 0.6 0.8 1.0

A D M 1 A D M 2

N S d i s t r i b u t i

• n

1 B *

CDF

1.0

No implosion ADM1: Neutron Stars Implode 3 Gyr after birth for GeV/cm3 dark mater ADM2: same, but 15 Gyr

Statistics of NS Mergers Located in Galaxies

• Use large sample of Kolmogorov-Smirnov tests to determine

how many NS mergers necessary to find dark matter

• Upper and lower quartile necessary to find dark matter

shown in right plot

Asymmetric Dark Matter Using NS Merger Locations in Galaxies

105 106 107 108 109 1010 1011 1.×10-48 1.×10-47 1.×10-46 1.×10-45 1.×10-44 1.×10-43 1.×10-42

mx (GeV) σnx (cm2)

MW Pulsars

X e n

• n

1 T

~10 NS Mergers

x e n

• n

S I ν f l

• r

~100 NS Mergers

Dark Matter Ignition of Type Ia Supernovae

• 1. Heavy asymmetric dark matter can collapse inside,

ignite, and explode white dwarfs.

• 2. There are interesting implications for the origin of

Type Ia Supernovae.

JB PRL 2015

Type Ia supernovae erupt when a portion of white dwarf becomes heated, igniting a thermonuclear flame-front that sweeps through the star, followed by an explosion. ignition nuclei fuse (56Ni) nuclei decay

days

l u m i n

• s

i t y

<- more ignition points

Maoz et al. 1312.0628 (Review), Olling et al. Nature 2015

Binary accretion ignition is now disfavored, by a lack of companion star "shocks" in SNIa light curves, along with the non-observation

• f H or He lines in any type Ia spectra. White dwarf mergers may

work, if the merger rate can match the high rate of type Ias.

It is not clear what ignites type Ia supernovae. Candidates include binary accretion to criticality (a.k.a. Chandrasekhar mass), and white dwarfs merging.

implied shocks not seen

Long tail of sub-Chandrasekhar mass SNIa

1408.6601

Mej M = (1.322 ± 0.022) + (0.185 ± 0.018)x1, x1 = [−3, 2]

The existence of sub-Chandrasekhar supernovae presents a quandary that binary accretion has trouble accounting for.

In order to ignite a carbon-oxygen white dwarf, the dark matter must be heavy so that it thermalizes inside a small volume within the white dwarf, and collects to the point of self-gravitation within ~1010 years. DM collects to the point of self-gravitation. Heavy Dark Matter Ignition of Type Ia Supernovae

In order to ignite a carbon-oxygen white dwarf, the dark matter must be heavy so that it thermalizes inside a small volume within the white dwarf, and collects to the point of self-gravitation within ~1010 years. DM collects to the point of self-gravitation. Heavy Dark Matter Ignition of Type Ia Supernovae

Harmonic Oscillator potential

kBT ∼ Gρwdmxr2

th

In order to ignite a carbon-oxygen white dwarf, the dark matter must be heavy so that it thermalizes inside a small volume within the white dwarf, and collects to the point of self-gravitation within ~1010 years. DM collapses, shedding gravitational potential energy by scattering with nuclei, igniting a supernova. DM collects to the point of self-gravitation. Heavy Dark Matter Ignition of Type Ia Supernovae

Harmonic Oscillator potential

kBT ∼ Gρwdmxr2

th

As it collapses to its minimum energy state, the dark matter will shed gravitational potential energy. For ignition to occur, at a given temperature, the speed of nuclear burning across a fixed region must exceed the white dwarf’s electron conduction diffusion rate. ignition

Timmes & Woosley 1992

Vector Portal Model

x

A A’

L = LSM + |DµΦ|2 − V (Φ) − 1 4F 02

µν + ✏A0 µ@νF µν + ¯

X(iDµµ − mX)X

Javier Acevedo, JB 2019

• 4
• 3
• 2
• 1

1 2 3

• 10
• 8
• 6
• 4
• 2

mX= 1010 GeV mX= 108 GeV mX= 1012 GeV

Log(mγ) [GeV] Log(εγ)

Dark photon mediator model

mX= 1014 GeV EXCLUDED

αx = 0.1 t = 3 Gyr Mwd = 1.4 M⨀

less massive WD, DM collapses later more massive WD, DM collapses sooner

Nsg ∼ T 3/2

w

m5/2

X ρ1/2 w

A more massive white dwarf is denser, so dark matter collects into a smaller ball, and collapses sooner. Altogether, this shortens the time for dark matter collapse in more massive white dwarfs.

(more) DM collapses later (less) DM collapses sooner

Line Mw /M Rw /(103 km) ρw /(107 g/cm3) 1.4 2.5 100 1.3 3 40 1.1 5 6 0.9 6 2 DM Collapse Tw = 107 K

X E N O N / L U X S I

(σnX/cm2) (mX/GeV) Line tw/Gyr 5 0.5

105 106 107 108 10-44 10-43 10-42 10-41 10-40 10-39 10-38

The limiting factor for heavy DM-induced-ignition of white dwarfs is the mass of the DM particle. Heavier DM collapses after fewer particles have collected, and fewer collapsing particles transfer less heat.

Line Mw /M Rw /(103 km) ρw /(107 g/cm3) 1.4 2.5 100 1.3 3 40 1.1 5 6 0.9 6 2 (σnX/cm2) (mX/GeV) Line tw/Gyr 5 0.5 DM Ignition Tw = 107 K

X E N O N / L U X S I

105 106 107 108 10-43 10-42 10-41 10-40 10-39 10-38

Sensitivity to high mass dark matter below current limits.

There is an unexplained correlation between the age of type Ia supernovae host galaxies, and the "stretch" of the type Ia

• lightcurve. Note that, as we saw earlier, type Ia stretch

correlates with type Ia progenitor white dwarf mass.

1311.6344

Host galaxy age correlates with stretch SNIadm

Data on the mass of type Ias inferred from luminosity

1408.6601

Data on the ages of stars adjacent to type Ia supernovae

1311.6344

Log(Age/Gyr) (MSN1a /M) SNIa progenitor age versus mass

bin1 bin2

DM mass σnX/cm2 10 PeV 3×10-42

100 PeV 2×10-42

0.0 0.5 1.0 1.0 1.2 1.4 1.6

Interesting trend — more massive WDs explode sooner.

DM collects Two New Heavy Dark Matter White Dwarf Ignition Mechanisms DM collapses

1. No ignition during collapse. 2. Small black hole forms.

• 3. Evaporating black hole ignites WD.

A. Strong Ignition B. Hawking Ignition

• 1. Higher dark matter

cross-section than required for collapse causes ignition

6 8 10 12 14 16 18

• 45
• 40
• 35
• 30

X e n

• n
• 1

T

σnX ignition NS implosions

Log(mX) [GeV] Log(σnX) [cm2]

WD parameters: M = 1.4 M R = 2.5 x 103 km ρwd = 109 g/cm3

BH evaporation ignition S e l f

• g

r a v

6 8 10 12 14 16 18

• 45
• 40
• 35
• 30

X e n

• n
• 1

T

σnX ignition NS implosions

Log(mX) [GeV] Log(σnX) [cm2]

WD parameters: M = 1.4 M R = 2.5 x 103 km ρwd = 109 g/cm3

BH evaporation ignition S e l f

• g

r a v

Javier Acevedo

6 8 10 12 14 16 18

• 45
• 40
• 35
• 30

X e n

• n
• 1

T

σnX ignition NS implosions

Log(mX) [GeV] Log(σnX) [cm2]

WD parameters: M = 1.4 M R = 2.5 x 103 km ρwd = 109 g/cm3

BH evaporation ignition S e l f

• g

r a v

Cool parameter space: implodes GC pulsars, type Ia progenitor solution, can be found at next-gen direct detection.

Thanks!