D-Net

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    <dc:creator>Bousso, Raphael</dc:creator>

    <dc:creator>Freivogel, Ben</dc:creator>

    <dc:creator>Leichenauer, Stefan</dc:creator>

    <dc:dateAccepted>2010-03-15</dc:dateAccepted>

    <dc:description>  The covariant entropy bound states that the entropy, S, of matter on a

light-sheet cannot exceed a quarter of its initial area, A, in Planck units.

The gravitational entropy of black holes saturates this inequality. The entropy

of matter systems, however, falls short of saturating the bound in known

examples. This puzzling gap has led to speculation that a much stronger bound,

S< A^{3/4}, may hold true. In this note, we exhibit light-sheets whose entropy

exceeds A^{3/4} by arbitrarily large factors. In open FRW universes, such

light-sheets contain the entropy visible in the sky; in the limit of early

curvature domination, the covariant bound can be saturated but not violated. As

a corollary, we find that the maximum observable matter and radiation entropy

in universes with positive (negative) cosmological constant is of order

Lambda^{-1} (Lambda^{-2}), and not |Lambda|^{-3/4} as had hitherto been

believed. Our results strengthen the evidence for the covariant entropy bound,

while showing that the stronger bound S< A^{3/4} is not universally valid. We

conjecture that the stronger bound does hold for static, weakly gravitating

systems.

</dc:description>

    <dc:description>Comment: 36 pages, 10 figures</dc:description>

    <dc:identifier>http://arxiv.org/abs/1003.3012</dc:identifier>

    <dc:language>eng</dc:language>

    <dc:title>Saturating the holographic entropy bound</dc:title>

    <dc:subject>High Energy Physics - Theory</dc:subject>

    <dc:subject>Astrophysics - Cosmology and Extragalactic Astrophysics</dc:subject>

    <dc:subject>General Relativity and Quantum Cosmology</dc:subject>

    <dc:subject>High Energy Physics - Phenomenology</dc:subject>

    <dr:CobjCategory>0001</dr:CobjCategory>

    <dr:CobjIdentifier>Phys.Rev.D82:084024,2010</dr:CobjIdentifier>

    <dr:CobjIdentifier>doi:10.1103/PhysRevD.82.084024</dr:CobjIdentifier>

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    <oaf:identifier identifierType="doi">10.1103/PhysRevD.82.084024</oaf:identifier>

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