21cm Hydrogen spectrum anomaly and dark matter Qiaoli Yang Jian University Phys.Rev.Lett. 121 (2018) 111301 Nick Houston, Chuang Li, Tianjun Li, Qiaoli.

Slides:



Advertisements
Similar presentations
PHY306 1 Modern cosmology 3: The Growth of Structure Growth of structure in an expanding universe The Jeans length Dark matter Large scale structure simulations.
Advertisements

1 The structure and evolution of stars Lecture 3: The equations of stellar structure Dr. Stephen Smartt Department of Physics and Astronomy
Major Epochs in the Early Universe t3x10 5 years: Universe matter dominated Why? Let R be the scale length.
Axion BEC Dark Matter Pierre Sikivie Vistas in Axion Physics Seattle, April 22-26, 2012 Collaborators: Ozgur Erken, Heywood Tam, Qiaoli Yang.
Plasma Astrophysics Chapter 3: Kinetic Theory Yosuke Mizuno Institute of Astronomy National Tsing-Hua University.
Sussex The WIMP of a minimal walking Technicolor Theory J. Virkajärvi Jyväskylä University, Finland with K.Kainulainen and K.Tuominen.
PRESENTATION TOPIC  DARK MATTER &DARK ENERGY.  We know about only normal matter which is only 5% of the composition of universe and the rest is  DARK.
Particle Physics and Cosmology
Particle Physics and Cosmology Dark Matter. What is our universe made of ? quintessence ! fire, air, water, soil !
Functional renormalization – concepts and prospects.
QCD – from the vacuum to high temperature an analytical approach an analytical approach.
Scalar dispersion forces, BE condensation and scalar dark matter J A Grifols, UAB Valparaíso, December 11-15, 2006.
The Cosmological Constant and Technical Naturalness Sunny Itzhaki hep-th/ work to appear.
On the Distribution of Dark Matter in Clusters of Galaxies David J Sand Chandra Fellows Symposium 2005.
Prof. Eric Gawiser Galaxy Formation Seminar 2: Cosmological Structure Formation as Initial Conditions for Galaxy Formation.
The Galaxy Formation Paradigm Paradigm R. Giovanelli Astro620/Spring ‘07 Remember to mention.pdf file.
Refining the free function of MOND Workshop Program Dark Matter and Alternative Gravities.
Physics of fusion power Lecture 7: particle motion.
Different physical properties contribute to the density and temperature perturbation growth. In addition to the mutual gravity of the dark matter and baryons,
Cosmological Reconstruction via Wave Mechanics Peter Coles School of Physics & Astronomy University of Nottingham.
 It would appear that there is more matter in the universe, called dark matter, than we see. We believe this because  The edges of galaxies are rotating.
Dark Matter and Dark Energy Just because something is unknown does not make it unknowable 1.
Components of the Milky Way The light from galaxies is centrally concentrated. But is the mass also centrally concentrated? Does Mass follow Light in Galaxies?
Robert Foot, CoEPP, University of Melbourne June Explaining galactic structure and direct detection experiments with mirror dark matter 1.
Dark Matter and Dark Energy from the solution of the strong CP problem Roberto Mainini, L. Colombo & S.A. Bonometto Universita’ di Milano Bicocca Mainini.
The Cosmic Microwave Background Lecture 2 Elena Pierpaoli.
Bose-Einstein Condensation of Dark Matter Axions Pierre Sikivie (U. of Florida) Center for Particle Astrophysics Fermilab, August 6, 2009.
Varying fundamental constants - a key property and key problem of quintessence.
The Universe  What do we know about it  age: 14.6 billion years  Evolved from Big Bang  chemical composition  Structures.
QED at Finite Temperature and Constant Magnetic Field: The Standard Model of Electroweak Interaction at Finite Temperature and Strong Magnetic Field Neda.
by Silke Weinfurtner, Matt Visser and Stefano Liberati Massive minimal coupled scalar field from a 2-component Bose-Einstein condensate ESF COSLAB Network.
An argument that the dark matter is axions Pierre Sikivie Miami 2013 Conference Fort Lauderdale, December 16, 2013 Collaborators: Ozgur Erken, Heywood.
Bose-Einstein Condensation of Dark Matter Axions Pierre Sikivie ASK2011 Conference Seoul, Korea April 11, 2011.
Possible Evidence of Thermodynamic Activity in Dark Matter Haloes.
Lecture III Trapped gases in the classical regime Bilbao 2004.
Vlasov Equation for Chiral Phase Transition
Dark Matter and Dark Energy. Most of the universe is dark matter and dark energy. Most of the mass-energy, about 95%, in the universe is ‘dark’. By dark.
A Lightning Review of Dark Matter R.L. Cooper
Bose-Einstein Condensation of Dark Matter Axions
Bose-Einstein Condensation of Dark Matter Axions Pierre Sikivie COSMO/CosPA 2010 Conference The University of Tokyo September 27 - October 1, 2010.
Holographic QCD in the medium
LUMINOUS MATTER  luminous = »The matter that astronomers see in the Universe (stars, dust clouds, etc.) makes up less than 1/2 of one percent of.
Bose-Einstein Condensation of Dark Matter Axions Pierre Sikivie Miami 2011 Conference Fort Lauderdale, December 19, 2011 Collaborators: Ozgur Erken, Heywood.
Dark Matter and Dark Energy from the solution of the strong CP problem Roberto Mainini, L. Colombo & S.A. Bonometto Universita’ di Milano Bicocca Mainini.
An argument that the dark matter is axions Pierre Sikivie IPTh seminar Saclay, 11 Juin, 2015 Collaborators: Ozgur Erken, Heywood Tam, Qiaoli Yang Nilanjan.
Gauge/gravity duality in Einstein-dilaton theory Chanyong Park Workshop on String theory and cosmology (Pusan, ) Ref. S. Kulkarni,
Derek F. Jackson Kimball. Collaboration Dmitry Budker, Arne Wickenbrock, John Blanchard, Samer Afach, Nathan Leefer, Lykourgas Bougas, Dionysis Antypas.
Konstantinos Dimopoulos Lancaster University Work done with: Sam Cormack arXiv: [astro-ph.HE]
Astrophysics – final topics Cosmology Universe. Jeans Criterion Coldest spots in the galaxy: T ~ 10 K Composition: Mainly molecular hydrogen 1% dust EGGs.
Spherical Collapse and the Mass Function – Chameleon Dark Energy Stephen Appleby, APCTP-TUS dark energy workshop 5 th June, 2014 M. Kopp, S.A.A, I. Achitouv,
Quantum Mechanical Models for Near Extremal Black Holes
THE ISOTOPIC FOLDY-WOUTHUYSEN REPRESENTATION
Axion Electrodynamics
Quantum optics Eyal Freiberg.
Collective Excitations in QCD Plasma
TeV-Scale Leptogenesis and the LHC
NGB and their parameters
Cyrille Marquet Columbia University
Chapter 3 Plasma as fluids
dark matter Properties stable non-relativistic non-baryonic
Weak Interacting Holographic QCD
Ch 2 - Kinetic Theory reinisch_
Effective gravitational interactions of dark matter axions
Primordial BHs.
Kinetic Theory.
Shintaro Nakamura (Tokyo University of Science)
Kinetic Theory.
The Case for Axion Dark Matter
Axion Like Particle and the CMB Asymmetry
Presentation transcript:

21cm Hydrogen spectrum anomaly and dark matter Qiaoli Yang Jian University Phys.Rev.Lett. 121 (2018) 111301 Nick Houston, Chuang Li, Tianjun Li, Qiaoli Yang, Xin Zhang. Phys.Rev.Lett. 108 (2012) 061304 O. Erken, P. Sikivie, H. Tam, Q. Yang. Phys.Rev.Lett. 103 (2009) 111301 P. Sikivie, Q. Yang.

Dark Ages picture by NASA

21 cm transition

Spin temperature  

Dark Ages Rep. Prog. Phys. 75, 086901 (2012), J. Pritchard, A. Loeb.

The EDGES anomaly  

Cold Dark Matter (CDM) CDM is widely believed to be an important part of the universe based on a large number of observations: Dynamics of galaxy clusters. Rotation curves of galaxies. Abundance of light elements. Gravitational lensing. Anisotropies of the CMBR.

CDM Accounts 23% of total energy density of universe while baryonic matter accounts 4%. Properties: a. Pressureless Primordial velocity is very small , at most ~ today . b.Collisionless Cold dark matter is weakly interacting (so dark), except for gravity.

Axion Properties Introduced to solve the strong CP problem of the standard model. In QCD, a formally total divergence term cannot be neglected due to the instanton solutions. This term violates CP invariance if The measurement of electric dipole moment of neutron gives a upper limit:

where relaxes to zero. A pseudo-Nambu-Goldstone boson is produced To solve the strong CP problem, one introduces a new U(1) symmetry that is spontaneously broken where relaxes to zero. A pseudo-Nambu-Goldstone boson is produced

After QCD phase transition, the “PQ” Nambu-Goldstone boson acquires mass due to instanton effects, hence becoming a quasi-Nambu-Goldstone boson, the “axion”. Axion models: PQWW, KSVZ, DFSZ. Axion like particles (ALPs) can also arise from string compactifications.

Cold axion properties Small velocity dispersion: . High physical space density:

Cold axion properties High phase space density due to 1&2: Particles number is effectively conserved:

Cold axions form BEC if they thermalize BEC results from the impossibility to allocate additional charges to the excited states for given temperature. Axion particle number is effectively conserved and is the relevant charge. Cold axions’ effective temperature is below the critical temperature which is very high due to axions high number density.

axion BEC in three arenas: 1. in the linear regime within the horizon. 2. in the non-linear regime within the horizon. 3. upon entering the horizon.

Axion BEC in the linear regime within horizon. From first order of density perturbation theory within the horizon, we get: where

This implies a nonzero Jeans length compared with the collisionless DM. From equation above, one gets:

The equation of motion in non-linear regime within horizon:

In the galactic halos BEC has the property by appearance of vortices. BEC is consistent with small scale structures.

Most many particle systems are in the particle kinetic regime where: The cold axions are in the opposite regime: Let us call it “condensed regime”.

The question is: starting with an arbitrary initial state, how quickly will the average axion state occupation numbers approach a thermal distribution?

We derive evolution equations for the out of equilibrium system, as an expansion in powers of the coupling strength. The first order terms average to zero in the kinetic regime. The second order terms yield the ordinary Boltzmann equation.

The axions can be written: The Hamiltonian is

Solve the Heisenberg equation perturbatively, where: . One gets:

The second order terms yield the Boltzmann equation The second order terms yield the Boltzmann equation. The first order terms, along with the off diagonal second terms average to zero in the “kinetic regime”. In the condensed regime, the first order terms no longer average to zero and dominate. Considering the high occupation numbers of axion states, we can replace the operator A, A+ with complex numbers whose magnitude is of order .

We get a c-number equation: which lead to the thermalization rate : for the gravitational interaction.