Academia.eduAcademia.edu

Figure 3 – uploaded by Sayantan Choudhury

See full PDFdownloadDownload figure
where we have used the (¢ — ¢9) < Mp (including at @ = demp and ¢ = ¢-) around ¢o. All the leading or- der dimensionful Planck scale suppressed expansion co- efficients (C,) and (D,) are given in terms of the model parameters (a, 8,7,«), which are mentioned in the ap- pendix.

Figure 3 where we have used the (¢ — ¢9) < Mp (including at @ = demp and ¢ = ¢-) around ¢o. All the leading or- der dimensionful Planck scale suppressed expansion co- efficients (C,) and (D,) are given in terms of the model parameters (a, 8,7,«), which are mentioned in the ap- pendix.

Related Figures (2)

and Eq. (1), we can derive a simple expression for the tensor-to-scalar ratio, r, as: where Cg = 4(In2+ ye) — 5 with yg = 0.5772 is the Euler-Mascheroni constant. Here the slow-roll parame- ters are given by in terms of the inflationary potential V(@), which can be expressed as:
and Eq. (1), we can derive a simple expression for the tensor-to-scalar ratio, r, as: where Cg = 4(In2+ ye) — 5 with yg = 0.5772 is the Euler-Mascheroni constant. Here the slow-roll parame- ters are given by in terms of the inflationary potential V(@), which can be expressed as:
In order to perform the momentum integration we use the tensor-to-scalar ratio r(k&) at any arbitrary momen- tum scale, which can be expressed as:
In order to perform the momentum integration we use the tensor-to-scalar ratio r(k&) at any arbitrary momen- tum scale, which can be expressed as:
Related topics:
RoboticsMathematicsMathematical PhysicsObservational AstronomyGravitational AstronomyPhilosophyCosmology (Physics)GravitationParticle PhysicsTheoretical astrophysics
580 California St., Suite 400
San Francisco, CA, 94104
© 2025 Academia. All rights reserved