Note on Tsallis holographic dark energy in Brans–Dicke cosmology
Anil Kumar Yadav
Abstract
Abstract In this paper, we have investigated that the power law variation of Brans–Dicke scalar field $$(\phi )$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:mo>(</mml:mo> <mml:mi>ϕ</mml:mi> <mml:mo>)</mml:mo> </mml:mrow> </mml:math> with scale factor ( a ) is not validated by field equations in general for the Universe filled with dark matter and Tsallis type holographic dark energy. However, for specific choice of free parameters $$(\omega = -\frac{3}{2}$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:mo>(</mml:mo> <mml:mi>ω</mml:mi> <mml:mo>=</mml:mo> <mml:mo>-</mml:mo> <mml:mfrac> <mml:mn>3</mml:mn> <mml:mn>2</mml:mn> </mml:mfrac> </mml:mrow> </mml:math> and $$n = -1)$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:mi>n</mml:mi> <mml:mo>=</mml:mo> <mml:mo>-</mml:mo> <mml:mn>1</mml:mn> <mml:mo>)</mml:mo> </mml:mrow> </mml:math> which are differ from its values fixed in Ghaffari et al. (Eur Phys J C 78:706, 2018) to describe various physical properties of the Universe in derived model, the power law variation of $$\phi $$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mi>ϕ</mml:mi> </mml:math> with a leads to consistent results. Further, we notice that the energy conservation law for Tsallis holographic dark energy in Brans–Dicke gravity does not hold.