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SUMMARY:Dark energy due to quantum corrections to effective potential
DTSTART;VALUE=DATE-TIME:20241022T140500Z
DTEND;VALUE=DATE-TIME:20241022T160000Z
DTSTAMP;VALUE=DATE-TIME:20261014T224957Z
UID:indico-contribution-4145@cern.ch
DESCRIPTION:Speakers: Vladislav Filippov (Bogoliubov Laboratory of Theoret
 ical Physics\, Joint Institute for Nuclear Research\, Dubna\, Russia)\nInf
 lationary expansion is one of the most promising models allowing one to de
 scribe the properties of the early Universe and its later development. In 
 the simplest realisation of the inflationary scenario\, it is generally as
 sumed that after the Universe leaves the inflationary stage and post-infla
 tionary reheating\, it remains at minimum potential with a value of $\\Lam
 bda \\sim 10^{-47}$ GeV$^{4}$ or $10^{-120}$ in Planck units.\n\nIn this w
 ork\, we show that quantum corrections to some cosmological models [1\,2] 
 can lead to a significant modification of the behaviour of the initial pot
 ential and the appearance of a non-zero ground state energy of the Univers
 e which can be interpreted as a cosmological constant.\n\nWe apply the for
 malism of the effective potential to the simplest forms of $\\alpha$-attra
 ctors which can be represented by the so-called $T$-models and $E$-models 
 [3]. However\, simpler models\, say\, such as arbitrary degree potentials\
 , we have considered in [1].\n\nWe derived the generalised renormalisation
  group (RG) equations that sum up the whole sequence of leading logarithmi
 c contributions to the effective potential. As a result\, the accounting o
 f quantum corrections leads to a change of character and a lift of the eff
 ective potential [4\,5]. We interpreted this uplift as the appearance of t
 he cosmological constant $\\Lambda$ for the $T^{2}$ and $E^{2}$ models.\n\
 nThus\, we have found out that the cosmological constant $\\Lambda$ may ex
 ist as a consequence of quantum corrections to the effective potential  wi
 th some value of the scale transmutation parameter $\\mu$ even in non-reno
 rmalizable models of inflation. And the value of the cosmological constant
  $\\Lambda$ allows one to fix the parameter $\\mu$ which is a free paramet
 er in the non-renormalizable theory.\n\n[1] D. I. Kazakov\, R. M. Iakhibba
 ev\, and D. M. Tolkachev. Leading all-loop quantum contribution to the eff
 ective potential in general scalar field theory. JHEP\, 04:128\,2023.\n\n[
 2] D. I. Kazakov\, R. M. Iakhibbaev\, and D. M. Tolkachev. Leading all-loo
 p quantum contribution to the effective potential in the inflationary cosm
 ology. JCAP\, 09:049\,2023.\n\n[3] Renata Kallosh\, Andrei Linde\, and Die
 derik Roest. Superconformal Inflationary $\\alpha$ -Attractors. JHEP\, 11:
 198\, 2013.\n\n[4] Tolkachev D. M.\, Kazakov D. I.\, Iakhibbaev R. M.\, an
 d Filippov V. A. Quantum corrections to effective potentials of simplest 
 𝛼-attractors. PoS\, ICPPCRubakov2023:022\,2024.\n\n[5] D. I. Kazakov\, 
 R. M. Iakhibbaev\, D. M. Tolkachev\, and V. A. Filippov. Dark energy due t
 o quantum corrections to effective potential. *In preparation*.\n\nhttps:/
 /indico.particle.mephi.ru/event/436/contributions/4145/
LOCATION: Alexeevskiy hall
URL:https://indico.particle.mephi.ru/event/436/contributions/4145/
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