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SUMMARY:Constraining the Phase Space for Chameleon Dark Energy
DTSTART;VALUE=DATE-TIME:20110714T121500Z
DTEND;VALUE=DATE-TIME:20110714T123000Z
DTSTAMP;VALUE=DATE-TIME:20231205T181345Z
UID:indico-contribution-5210@events.saip.org.za
DESCRIPTION:Speakers: Muzikayise Sikhonde (University of Cape Town)\nA num
ber of solutions to the dark energy problem have been proposed in literatu
re\, the simplest is the cosmological constant Λ. But the cosmological co
nstant lacks theoretical explanation for its extremely small value\, thus
dark energy is more generally modeled as quintessence scalar field rolling
down a flat potential. For the quintessence scalar field to be evolving o
n\ncosmological scales to day its mass must be of order H0 \, which is the
present value of the Hubble constant. A scalar field φ whose mass varies
with the background energy density was proposed by Khoury and Weltman(200
3). This scalar field can evolve cosmologically while having coupling (β)
to different matter fields of order unity. Such a scalar field also coupl
es to photons in the presence of an external magnetic field via the φF2 i
nteraction\, where F stands for the electromagnetic field strength tensor.
The chameleon(φ)-photon coupling of this nature causes a conversion of p
hotons to light Chameleon(φ) particles and vice versa. In this work we in
vestigate this effect on pulsars\, and we constrain the parameter space of
this theory.\n\nhttps://events.saip.org.za/event/7/contributions/5210/
LOCATION: Acro2
URL:https://events.saip.org.za/event/7/contributions/5210/
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