Slow-roll inflation in the presence of a dark energy coupling

In models of coupled dark energy, in which a dark energy scalar field couples to other matter components, it is natural to expect a coupling to the inflaton as well. We explore the consequences of such a coupling in the context of single-field slow-roll inflation. Assuming an exponential potential for the quintessence field we show that the coupling to the inflaton causes the quintessence field to be attracted toward the minimum of the effective potential. If the coupling is large enough, the field is heavy and is located at the minimum. We show how this affects the expansion rate and the slow-roll of the inflaton field, and therefore the primordial perturbations generated during inflation. We further show that the coupling has an important impact on the processes of reheating and preheating.

[1]  The Cosmon model for an asymptotically vanishing time dependent cosmological 'constant' , 1994, hep-th/9408025.

[2]  A. Riotto.  Inflation and the theory of cosmological perturbations , 2002, hep-ph/0210162.

[3]  M. Trodden,et al.  Constraining Interactions in Cosmology's Dark Sector , 2008, 0808.1105.

[4]  Starobinsky,et al.  Reheating after inflation. , 1994, Physical review letters.

[5]  Coupled Quintessence , 1999, astro-ph/9908023.

[6]  Andrei Linde,et al.  Towards the theory of reheating after inflation , 1997 .

[7]  D. Mota,et al.  Detecting chameleons through Casimir force measurements , 2007, 0709.2075.

[8]  Jérôme Martin.  QUINTESSENCE: A MINI-REVIEW , 2008, 0803.4076.

[9]  Shinji Tsujikawa,et al.  Dynamics of dark energy , 2006 .

[10]  C. Wetterich.  COSMOLOGY AND THE FATE OF DILATATION SYMMETRY , 1988, 1711.03844.

[11]  A. Liddle,et al.  Initial conditions for quintessence after inflation , 2002, astro-ph/0203232.

[12]  D. Stojkovic,et al.  Electroweak vacua, collider phenomenology, and possible connection with dark energy , 2009 .

[13]  S. D. Odintsov,et al.  INTRODUCTION TO MODIFIED GRAVITY AND GRAVITATIONAL ALTERNATIVE FOR DARK ENERGY , 2006, hep-th/0601213.

[14]  M. Halpern,et al.  FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: LIKELIHOODS AND PARAMETERS FROM THE WMAP DATA , 2008, 0803.0586.

[15]  Michael S. Turner,et al.  The early Universe , 1981, Nature.

[16]  L. Amendola,et al.  Quintessence cosmologies with a growing matter component , 2008 .

[17]  R. Brandenberger,et al.  Preheating with non-standard kinetic term , 2008, 0808.0936.

[18]  Viatcheslav Mukhanov,et al.  Physical Foundations of Cosmology: Preface , 2005 .

[19]  G. Starkman,et al.  Dark energy, colored anti-de Sitter vacuum, and the CERN Large Hadron Collider phenomenology , 2008 .

[20]  P. Peebles,et al.  Cosmological consequences of a rolling homogeneous scalar field. , 1988, Physical review. D, Particles and fields.

[21]  Mark Trodden,et al.  Cosmology of generalized modified gravity models , 2005 .

[22]  D. Mota,et al.  Testing Chameleon Theories with Light Propagating through a Magnetic Field , 2007, 0707.2801.

[23]  T. Dent,et al.  Time variation of fundamental couplings and dynamical dark energy , 2008, 0809.4628.