Novel searches for dark matter and fifth- forces with ... ?· Yevgeny Stadnik, Victor Flambaum Novel…

Download Novel searches for dark matter and fifth- forces with ... ?· Yevgeny Stadnik, Victor Flambaum Novel…

Post on 16-Jun-2018

212 views

Category:

Documents

0 download

Embed Size (px)

TRANSCRIPT

  • Yevgeny Stadnik, Victor Flambaum

    Novel searches for dark matter and fifth-

    forces with atomic clock spectroscopy,

    laser interferometry and pulsar timing

    Helmholtz Institute Mainz, Germany

    University of New South Wales, Sydney, Australia

    52nd Rencontres de Moriond Gravitation, La Thuile, March 2017

    PRL 113, 081601 (2014); PRL 113, 151301 (2014);

    PRL 114, 161301 (2015); PRL 115, 201301 (2015);

    PRL 117, 271601 (2016);

    PRD 89, 043522 (2014); PRD 90, 096005 (2014);

    EPJC 75, 110 (2015); PRA 93, 063630 (2016);

    PRD 93, 115037 (2016); PRA 94, 022111 (2016).

    In collaboration with: Dmitry Budker (Helmholtz Institute Mainz)

  • Motivation Overwhelming astrophysical evidence for existence

    of dark matter (~5 times more dark matter than

    ordinary matter).

  • Motivation Overwhelming astrophysical evidence for existence

    of dark matter (~5 times more dark matter than

    ordinary matter).

    What is dark matter and how does it interact with ordinary matter non-gravitationally?

  • Motivation Traditional scattering-off-nuclei searches for

    heavy WIMP dark matter particles () have not yet produced a strong positive result.

  • Motivation Traditional scattering-off-nuclei searches for

    heavy WIMP dark matter particles () have not yet produced a strong positive result.

    Problem: Observable is quartic in the interaction

    constant e, which is extremely small (e1 >> )!

  • n(dB/2)3 >> 1 * Coherently oscillating field => cold, i.e., E mc2

    Low-mass Spin-0 Dark Matter We propose to search for other well-motivated forms of dark

    matter: low-mass spin-0 particles, which form a coherently *

    oscillating classical field ( m202/2): (t) = 0 cos(mc2t/)

  • n(dB/2)3 >> 1 * Coherently oscillating field => cold, i.e., E mc2

    Low-mass Spin-0 Dark Matter We propose to search for other well-motivated forms of dark

    matter: low-mass spin-0 particles, which form a coherently *

    oscillating classical field ( m202/2): (t) = 0 cos(mc2t/) cosmic laser

  • n(dB/2)3 >> 1 * Coherently oscillating field => cold, i.e., E mc2

    Low-mass Spin-0 Dark Matter We propose to search for other well-motivated forms of dark

    matter: low-mass spin-0 particles, which form a coherently *

    oscillating classical field ( m202/2): (t) = 0 cos(mc2t/), via effects that are linear in the interaction constant .

  • n(dB/2)3 >> 1

    10-22 eV m 0.1 eV 10-8 Hz f 1013 Hz

    * Coherently oscillating field => cold, i.e., E mc2

    Low-mass Spin-0 Dark Matter We propose to search for other well-motivated forms of dark

    matter: low-mass spin-0 particles, which form a coherently *

    oscillating classical field ( m202/2): (t) = 0 cos(mc2t/), via effects that are linear in the interaction constant .

  • n(dB/2)3 >> 1

    10-22 eV m 0.1 eV 10-8 Hz f 1013 Hz Inaccessible to traditional scattering-off-nuclei and collider

    searches

    * Coherently oscillating field => cold, i.e., E mc2

    Low-mass Spin-0 Dark Matter We propose to search for other well-motivated forms of dark

    matter: low-mass spin-0 particles, which form a coherently *

    oscillating classical field ( m202/2): (t) = 0 cos(mc2t/), via effects that are linear in the interaction constant .

  • n(dB/2)3 >> 1

    10-22 eV m 0.1 eV 10-8 Hz f 1013 Hz Inaccessible to traditional scattering-off-nuclei and collider

    searches

    Ultra-low-mass spin-0 DM with mass m ~ 10-22 eV has been proposed to resolve several small-scale crises of the cold DM model (cusp-core problem and others)

    * Coherently oscillating field => cold, i.e., E mc2

    Low-mass Spin-0 Dark Matter We propose to search for other well-motivated forms of dark

    matter: low-mass spin-0 particles, which form a coherently *

    oscillating classical field ( m202/2): (t) = 0 cos(mc2t/), via effects that are linear in the interaction constant .

  • n(dB/2)3 >> 1

    10-22 eV m 0.1 eV 10-8 Hz f 1013 Hz Inaccessible to traditional scattering-off-nuclei and collider

    searches

    Ultra-low-mass spin-0 DM with mass m ~ 10-22 eV has been proposed to resolve several small-scale crises of the cold DM model (cusp-core problem and others)

    f ~ 10-8 Hz (m ~ 10-22 eV) T ~ 1 year * Coherently oscillating field => cold, i.e., E mc2

    Low-mass Spin-0 Dark Matter We propose to search for other well-motivated forms of dark

    matter: low-mass spin-0 particles, which form a coherently *

    oscillating classical field ( m202/2): (t) = 0 cos(mc2t/), via effects that are linear in the interaction constant .

  • n(dB/2)3 >> 1

    Consideration of linear effects of dark matter in low-energy atomic and astrophysical phenomena has already allowed us

    to improve the sensitivity to some interactions of dark matter

    by up to 15 orders of magnitude (!)

    * Coherently oscillating field => cold, i.e., E mc2

    Low-mass Spin-0 Dark Matter We propose to search for other well-motivated forms of dark

    matter: low-mass spin-0 particles, which form a coherently *

    oscillating classical field ( m202/2): (t) = 0 cos(mc2t/), via effects that are linear in the interaction constant .

  • Low-mass Spin-0 Dark Matter

    Dark Matter

  • Low-mass Spin-0 Dark Matter

    Dark Matter

    Scalars:

    Even-parity

    Pseudoscalars

    (Axions, ALPs):

    Odd-parity

  • Low-mass Spin-0 Dark Matter

    Dark Matter

    Scalars:

    Even-parity

    Pseudoscalars

    (Axions, ALPs):

    Odd-parity

    Oscillating spin-dependent effects

    Slow evolution and oscillating variation of

    fundamental constants

  • Low-mass Spin-0 Dark Matter

    Dark Matter

    Scalars:

    Even-parity

    Slow evolution and oscillating variation of

    fundamental constants

  • Cosmological Evolution of the

    Fundamental Constants Diracs large numbers hypothesis: G 1/t

  • Cosmological Evolution of the

    Fundamental Constants Diracs large numbers hypothesis: G 1/t Values of fundamental constants cannot be predicted,

    but must be determined from experiment:

    e.g., (q2 = 0) 1/137 locally (in space and time)

  • Cosmological Evolution of the

    Fundamental Constants Diracs large numbers hypothesis: G 1/t Values of fundamental constants cannot be predicted,

    but must be determined from experiment:

    e.g., (q2 = 0) 1/137 locally (in space and time) Contemporary dark-energy-type models:

    Cosmological evolution of fundamental constants driven

    by (nearly) massless exotic boson that couples to matter

  • Cosmological Evolution of the

    Fundamental Constants Diracs large numbers hypothesis: G 1/t Values of fundamental constants cannot be predicted,

    but must be determined from experiment:

    e.g., (q2 = 0) 1/137 locally (in space and time) Contemporary dark-energy-type models:

    Cosmological evolution of fundamental constants driven

    by (nearly) massless exotic boson that couples to matter

    Can a cosmological evolution of the fundamental constants be driven by dark matter?

  • Dark Matter-Induced Cosmological

    Evolution of the Fundamental Constants

    Consider an oscillating classical scalar field,

    (t) = 0 cos(mt), that interacts with SM fields (e.g., a fermion f) via quadratic couplings in .

    [Stadnik, Flambaum, PRL 115, 201301 (2015)]

  • Dark Matter-Induced Cosmological

    Evolution of the Fundamental Constants

    Consider an oscillating classical scalar field,

    (t) = 0 cos(mt), that interacts with SM fields (e.g., a fermion f) via quadratic couplings in .

    [Stadnik, Flambaum, PRL 115, 201301 (2015)]

  • Dark Matter-Induced Cosmological

    Evolution of the Fundamental Constants

    Consider an oscillating classical scalar field,

    (t) = 0 cos(mt), that interacts with SM fields (e.g., a fermion f) via quadratic couplings in .

    [Stadnik, Flambaum, PRL 115, 201301 (2015)]

  • Dark Matter-Induced Cosmological

    Evolution of the Fundamental Constants

    Consider an oscillating classical scalar field,

    (t) = 0 cos(mt), that interacts with SM fields (e.g., a fermion f) via quadratic couplings in .

    [Stadnik, Flambaum, PRL 115, 201301 (2015)]

  • Dark Matter-Induced Cosmological

    Evolution of the Fundamental Constants

    Consider an oscillating classical scalar field,

    (t) = 0 cos(mt), that interacts with SM fields