New insights on the physics beyond the Standard Model from astrophysical observations

1
New insights on the physics beyond the Standard
Model from astrophysical observations
Maurizio Giannotti T8-LANL In collaboration
with V.Cirigliano, A.Friedland, A.Heger
2
Outline

• Introduction
• Stars and the standard model
• Stars and physics beyond the standard
  model
• Stars and TeV scale physics ?
• Some Examples
• Axion
• Stars and Extra-Dimensions (with
  A.Friedland )
• Massive stars and physics beyond the standard
  model
• (with V.Cirigliano, A.Friedland,
  A.Heger)
• - Massive stars and neutrino magnetic
  moment
• Does a non-vanishing magnetic moment
  influence
• the behavior of a massive star?
• For which range of masses?
• What are the induced effects and what is the
  sensitivity?
• What are the observational effects?

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Weak Interactions and Star Cooling
Role of weak interactions in stellar cooling.
Already in 1963 Bernstain, Ruderman and Feinberg
studied the effects of electromagnetic properties
of neutrinos for the cooling of the sun. Their
bound on the neutrino magnetic moment was better
than the experimental bound at that time.
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Weak Interactions and Star Cooling
IMPORTANT QUESTION What energy scale can be
tested in stars ?
Role of weak interactions in stellar cooling.
Already in 1963 Bernstain, Ruderman and Feinberg
studied the effects of electromagnetic properties
of neutrinos for the cooling of the sun. Their
bound on the neutrino magnetic moment was better
than the experimental bound at that time.
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Neutrinos Energy Loss
DDegenerate NDNondegenerate
From G Beaudet, V.Petrosian, E. Salpeter (1967)
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Neutrino Cooling in Stars
Standard Cooling photons and neutrinos Photon
cooling is relevant in the non-degenerate region,
below T5x108K
Non-degenerate plasma
Degenerate plasma
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Neutrino Cooling in Stars
Standard Cooling photons and neutrinos Photon
cooling is relevant in the non-degenerate region,
below T5x108K
Neutrino
Non-degenerate plasma
T108 K
Log10 e/erg g-1 s-1
Log10 r/g cm-3
Degenerate plasma
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Neutrino Cooling in Stars
Standard Cooling photons and neutrinos Photon
cooling is relevant in the non-degenerate region,
below T5x108K
Massive Stars T M2/3 r1/3
15 Solar Mass
HB
Red Giant
WhiteDwarf
SUN
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Example Axion and Stellar Evolution
T108 K
15 Solar Mass
/g cm-3
HB
Red Giant
WhiteDwarf
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Example Axion and Stellar Evolution
T108 K
No axion He-flash off center Axion He-flash in
the center
15 Solar Mass
/g cm-3
HB
Red Giant
Axion cooling 10, 100 and 1000 bigger than the
standard neutrino emission
WhiteDwarf
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New Physics and Stellar Evolution
In the early evolutionary stages of a massive
stars there is more axion production than in HB
HB
Best bound on axion-photon coupling
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Summary of the bounds
HADRONIC Axion Window
DFSZ
PQ-Scale
106 GeV
Red Giants (gae) Only for DFSZ axion
HB Stars (gag)
Terrestrial Experiments
Cosmology
Axion heavy Production damped
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Summary of the bounds
HADRONIC Axion Window
DFSZ
PQ-Scale
106 GeV
Red Giants (gae) Only for DFSZ axion
HB Stars (gag)
Terrestrial Experiments
Cosmology
TERRESTRIAL EXPERIMENTS The axion cannot
interact too much
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Summary of the bounds
HADRONIC Axion Window
DFSZ
PQ-Scale
106 GeV
Red Giants (gae) Only for DFSZ axion
HB Stars (gag)
Terrestrial Experiments
ASTROPHYSICS The axion is invisible
Cosmology
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Summary of the bounds
HADRONIC Axion Window
DFSZ
PQ-Scale
106 GeV
Red Giants (gae) Only for DFSZ axion
HB Stars (gag)
Terrestrial Experiments
COSMOLOGY The axion cannot be too invisible
Cosmology
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Summary axion bounds
HADRONIC Axion Window
DFSZ
PQ-Scale
106 GeV
Red Giants (gae) Only for DFSZ axion
HB Stars (gag)
Terrestrial Experiments
ASTROPHYSICS The axion is invisible
Cosmology
TERRESTRIAL EXPERIMENTS
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CAST (Non-Standard Axion)
From the CAST collaboration, Journal of
Cosmology and Astroparticle Physics, 02, 008, 2009
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Particles leaking in the extra dimensions
Extended RS Metric
If ngt0 Photon confinement on the brane S.
Dubovsky, V. Rubakov and P.Tinyakov, JHEP 0008
041 (2000)
Virtual photons can escape in the extra dimensions
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Orthopositronium decay and new physics
Orthopositronium -- electron-positron bound
state of spin1 It cannot decay in 2 photons
gt main decay rate is in 3 photons gt lifetime
(150 ns) longer than the corresponding spin 0
state (parapositronium) -- It is a clean bound
state of pure leptons gt non strong interaction,
only electromagnetic -- In fact, there is
also a little of weak interactions
Standard decay oPs --gt 3 g
This is so small than any measurable invisible
decay mode would be an indication of new
physics such as -- Invisible decay into
(infinite) extradimension -- Other possibilities
are Mirror World Invisible decay through
photon mirror-photon mixing, Invisible decay
into millicharged particles ......
See, e.g., A. Badertscheret al., Phys. Rev. D75
(2007).
The goal is
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Orthopositronium decay in the extra dimensions
Orthopositronium decay into the extra dimensions
(n2)
lt 10-8
Standard decay oPs --gt 3 g
This implies the bound n2 gt k 1
TeV comparable to the bounds from Lep and Z decay
width For ngt2 the bound is very weak (n3 gt
kgt20GeV). From Z decay width kgt 100 GeV for any n
REFERENCES Gninenko, Krasnikov, Rubbia,
Phys.Rev.D67 (2003) A. Badertscheret al.,
Phys. Rev. D75 (2007) Proceedings of the 2005
APS April Meeting, http//meetings.aps.org/link/B
APS.2005.APR.T12.7 Proceedings of the2006Joint
APS/JPSMeeting, http//tabletop.icepp.s.u-tokyo.a
c.jp/invisi/jps2006Hawaii.pdf
Non-standard decay oPs --gt g -gt extra dim
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Plasmon decay into the extra dimensions
The different photon polarizations in a plasma
behave like massive particles with mass
wpl They can decay into the extra
dimensions. We found
n number of extra compact dimensions
A. Friedland, M. Giannotti Phys.Rev.Lett.100
(2008).
We can now compute the energy loss and consider
what that would imply for different stars. The
strongest impact would be for Red Giant
stars The energy loss through photon decay into
the extra-dimensions would delay the ignition of
helium in the core of a RG. The new energy-loss
rate must not exceed the standard loss through
plasmon decay by more then a factor of 2-3.
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Plasmon decay into the extra dimensions and stars
n1
From RG stars Delay of the He-flash
n2
n3
The goodness of our result depends on the huge
ratio between the weak scale and the plasma
frequency
From HB stars (observed number ratio of HB/RG
stars) we find comparable results
n1
From SN87A Neutrino signal from SN87A
n2
n3
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Comments on the oPs experiment
A terrestrial experiments sensitive to the
invisible decay modes of the orthopositronium sh
ould have the following sensitivities in order to
provide an analogous bound on k
for RG stars
for HB stars
for SN87A
-- Our analysis shows that, for n2, the
sensitivity for the BR in the o-Ps experiment
should improve by about 13 orders of
magnitude to be competitive with the
astrophysical bounds. The SN bound requires
at least 8 orders of magnitude better sensitivity
for the BR than the present sensitivity of
the oPs experiment, for any n -- The experiment
can sill be interesting to test other physics
beyond the standard model such as mirror
world, millicharged particles etc.
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Mirror World oPs Experiment and Astrophysics
T. D. Lee and C. N. Yang, Phys. Rev. 104,
254(1956) I. Kobzarev et al., Sov. J. Nucl Phys.
3, 837 (1966)
Mirror World New sector of particles and fields
completely identical to ours Mirror particles
interact with ours through gravity There can be
other interactions between standard and mirror
particles, such as
between standard and mirror photons
e F F
B. Holdom, Phys. Lett. B 166, 196 (1986).
Bound from BBN elt3x10-8
E. D. Carlson and S. L. Glashow, Phys. Lett. B
193, 168 (1987)
oPs Experiment
Mirror oPs
oPs
Current bound from oPs experiment elt1.55x10-7 A.
Badertscheret al., Phys. Rev. D75 (2007)
Non-standard decay oPs --gt g -gt oPs
Standard decay oPs --gt 3 g
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Mirror World oPs Experiment and Astrophysics
T. D. Lee and C. N. Yang, Phys. Rev. 104, 254
(1956) I. Kobzarev et al., Sov. J. Nucl Phys. 3,
837 (1966)
Mirror World New sector of particles and fields
completely identical to ours Mirror particles
interact with ours through gravity There can be
other interactions between standard and mirror
particles, such as
between standard and mirror photons
e F F
B. Holdom, Phys. Lett. B 166, 196 (1986).
Bound from BBN elt3x10-8
E. D. Carlson and S. L. Glashow, Phys. Lett. B
193, 168 (1987)
Bounds from SN
S.Davidson and M.E.Peskin, Phys. Rev. 49,
2114 (1994) S.Davidson,S.Hannestad,G.Raffelt
JHEP 0005 003 (2000)
e
e
elt3x10-8
elt 10-9
This bound is a little optimistic
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Massive Stars and New Physics
Pair
Photo
Plasma
Bremsstrahlung
From A.Heger, A.Friedland, M.Giannotti,
V.Cirigliano (2008)
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The Onion
Final composition of a 15 Mo star (Solar
Metallicity)
From Woosley, Heger, Weaver, Rev Mod Phys, 74,
1015 (2002)
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The Onion
Why study the effects of new physics in massive
stars? They offer a very different environment
with respect to other stars Observations are
improving rapidly We cannot consistently run a
SN explosion simulation without knowing the
uncertainties induced by new physics in the
pre SN evolution
Final composition of a 15 Mo star (Solar
Metallicity)
From Woosley, Heger, Weaver, Rev Mod Phys, 74,
1015 (2002)
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Neutrino Magnetic Moment
Massive neutrinos are expected to have a
non-vanishing magnetic moment. The
experimental limit mnlt 10-10 mB is very weak
there are many orders of magnitude between this
and the SM prediction. Theories beyond the SM
predict higher values for the neutrino magnetic
moment Evidence that mn/mBgt10-19 would require
changes in the weak sector of the SM
R.Barbieri, G.Fiorentini, 1988 N. F. Bell et al,
2005 S. Davidson et al 2005 N. F. Bell et al, 2006
If 10-15 mB lt mnlt 10-10 mB is measured or
inferred by astrophysical considerations, it
would be a strong indication that neutrinos are
Majorana fermions.
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Neutrino Magnetic Moment Bounds
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Neutrino Energy Loss Testing Neutrinos magnetic
moment
Standard
Electromagnetically induced
Neutrino Photoproduction
Neutrino Pair Production
Plasmon Decay
At low energies, for all the neutrino processes
but the plasmon decay, the energy loss for the
electromagnetic and weak induced processes are
equal for mn10-10 mB, which is approximately
the experimental bound. In the case of plasmon
decay there is a non-trivial dependence on the
density
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Neutrino Magnetic Moment and Stars Cooling
mn 0
15 Solar Mass
HB
Red Giant
WhiteDwarf
SUN
From A.Heger, A.Friedland, M.Giannotti,
V.Cirigliano (2008)
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Neutrino Magnetic Moment and Stars Cooling
mn10-11 mB
15 Solar Mass
HB
Red Giant
WhiteDwarf
SUN
From A.Heger, A.Friedland, M.Giannotti,
V.Cirigliano (2008)
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Neutrino Magnetic Moment and Stars Cooling
mn5x10-11 mB
15 Solar Mass
HB
Red Giant
WhiteDwarf
SUN
From A.Heger, A.Friedland, M.Giannotti,
V.Cirigliano (2008)
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Star sensitivity to neutrino magnetic moment
mn / mB
Stars sensitivity to mn RGB mn 3-5
x10-12 mB WD mn 3-5 x10-12 mB HB
mn 15 x10-12 mB NS mn 100 x10-12
mB SUN mn 400 x10-12 mB
SUN
Lifetime
10-10
NS
Croust cooling
HB
Time of He-burning
RGB
WD
Cooling
Delay He-flash
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Massive Stars and Neutrino Magnetic Moment
mn 0
Pair
Photo
Plasma
Bremsstrahlung
From A.Heger, A.Friedland, M.Giannotti,
V.Cirigliano (2008)
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Massive Stars and Neutrino Magnetic Moment
mn10-11 mB
Pair
Photo
Plasma
Bremsstrahlung
From A.Heger, A.Friedland, M.Giannotti,
V.Cirigliano (2008)
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Massive Stars and Neutrino Magnetic Moment
mn5x10-11 mB
Pair
Plasma
Bremsstrahlung
From A.Heger, A.Friedland, M.Giannotti,
V.Cirigliano (2008)
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Massive Stars and Neutrino Magnetic Moment
mn5x10-11 mB
Pair
Plasma
Bremsstrahlung
From A.Heger, A.Friedland, M.Giannotti,
V.Cirigliano (2008)
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Massive Stars and Neutrino Magnetic Moment
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Massive Stars sensitivity to magnetic dipole
moment
Evolution of central temperature and density
M 15MO, mn 0
Log T K
M 12MO mn 0
M 12MO mn 5x10-11 mB
M 15MO mn 5x10-11 mB
Log r g cm-3
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Massive Stars sensitivity to magnetic dipole
moment
Evolution of central temperature and density
Log T K
mn 0
mn 2x10-11 mB
mn 5x10-11 mB
Log r g cm-3
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Massive Stars and Magnetic dipole Moment
12 MO, mn5x10-11 mB Pre SN
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Massive Stars and Magnetic dipole Moment
11.5 MO, mn5x10-11 mB Before detonation
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Massive Stars and Magnetic dipole Moment
9.3 MO, mn2x10-11 mB Before detonation
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Neutrino Magnetic Moment and the fate of Stars
of different masses
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Observations

• New kind of explosion
• - no neutron star
• no neutrinos
• More 56Ni and 56Co
• Different light curves

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Observations
Hints are accumulating that stars of initial
mass 8-9 Mo do end up as SN explosion Smartt et
al. (2004) Van Dyk et al. (2003) Van Dyk et al.
(2006) Smartt et al. (2008)
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Observations
SN 2008bk Progenitor observed with mass in this
range Smartt et al. (2008)
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Conclusions
-- Stars offer a variety of interesting
environments to test physics beyond the standard
model -- From astrophysics we can get invaluable
insights on the physics beyond the SM The
invisible axion is invisible because of
astrophysics The aim of orthopositronium
experiments should not be to find
extradimensions, but other kind of physics
beyond the standard model. The bounds
found in stars on the extradimensional models
which predict photon disappearance are
several million times better than the present
terrestrial experiments. -- Massive stars
seem to be more interesting for particle physics
than we thought! The sensitivity of massive
stars to magnetic moment is comparable to the
sensitivity of HB stars Observations are
improving at a fast pace They should be very
sensitive to axion-photon coupling The
response to new physics could be dramatic new
kind of explosions! Maybe they are a good
place to find new physics rather than test it!