The Inflationary Brane-Antibrane Universe

C.P. Burgess; D. Nolte; F. Quevedo; G. Rajesh; M. Majumdar; R.-J. Zhang

REVIEW

The Inflationary Brane-Antibrane Universe

C.P. Burgess, M. Majumdar, D. Nolte, F. Quevedo, G. Rajesh, R.-J. Zhang

High Energy Physics - Theory · Submitted 21 May 2001 · 21 references

Pith's verdict: Read it for the clean negative result in §2.4 and the quartic flat-point trick in §2.5, not for the 'computable potential' framing.

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arXiv IDhep-th/0105204 (version 3)

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CitationC.P. Burgess, D. Nolte, F. Quevedo, G. Rajesh, M. Majumdar, R.-J. Zhang. "The Inflationary Brane-Antibrane Universe." arXiv:hep-th/0105204 (2001). https://pith.science/paper/SXHWNXF3

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Worth your time, but read it for the two things it actually establishes rather than the framing in the abstract and §3. What's new: §2.4 is a clean negative result — with the string-theory β of Eq. 2.6, the brane-antibrane potential is too steep to slow-roll anywhere the 1/y^{d⊥-2} approximation holds, and the asymmetric-compactification escape fails too. Then §2.5 finds the one place it works: at the centre of a hypercubic torus cell the lattice-summed potential has vanishing first and second derivatives (Eq. 2.18), so the leading term is quartic and η = -3γ(z/r⊥)² is small for small z. That is a real observation, and n-1 = -3/N follows without touching COBE. The COBE match then fixes M_p r⊥ ≈ 1.3×10⁶, i.e. r⊥⁻¹ ~ 10¹² GeV. One number fitted, disclosed as such. Soft spots, in order of weight. The frozen-moduli assumption in §2.3 is load-bearing, and the stress-test is right that it is sharper than 'unknown physics': the same A = 2T_p V∥ that drives inflation is a linear term in the volume-modulus potential, so freezing it needs m_mod ≫ H and a small shift of the minimum. Nobody checks this. It is the standard η problem, and the lattice symmetry that protects the inflaton's quartic flatness does nothing for the volume modulus. Second, γ in Eq. 2.20 is never computed, so Eq. 2.24 and the T_rh ~ 10¹³ GeV of Eq. 3.2 are order-of-magnitude statements; 'computable potential' in §3 is a bit generous. Third, §3's cascade is qualitative and the authors say so themselves — I would not score it either way, but the 3-brane selection argument is a story, not a derivation. The disagreement with Dvali-Solganik-Shafi (ref. 11, still 'to appear') is a footnote, not a load-bearing citation. Who should read it: anyone working on string inflation or brane-gas cosmology. The negative result and the flat-point trick are both citable, and the paper is honest about what it has not done. Send it out.

Referee report

Significance

If the frozen-moduli assumption of §2.3 can be justified, this is a genuine step forward: an inflationary potential computed from string theory rather than postulated, with a falsifiable prediction n − 1 ≈ −3/N ≈ −0.05 and dn/dlnk ~ −10⁻³ for N ≈ 60 (Eq. 2.23), within reach of MAP and Planck. The symmetry argument for the vanishing of V″ at the cell centre (Eq. 2.18) is clean, checkable, and does not depend on the details of the lattice sum. The negative result of §2.4 — that string-strength brane–antibrane couplings are too steep for generic initial conditions — is stated plainly and is itself a useful contribution. The COBE normalization Eq. 2.24 is a one-parameter fit, disclosed as such, not a prediction dressed as a fit. The cascade picture of §3 is qualitative but generative.

Major objections (3)

[§2.3, Eqs. (2.8)–(2.10)] The authors flag as 'our most crucial assumption' that the compactification moduli V⊥, V∥, φ and the torus shape are frozen by 'some unknown physics,' and they are honest about it. What remains unresolved is the quantitative condition. The inflaton potential energy is A = 2T_p V∥ (Eq. 2.10), which is linear in V∥, so freezing V∥ requires a stabilization mass satisfying m_mod² ≫ H² = 2T_p V∥/(3M_p²) and a shift δV∥/V∥ ≈ 2T_p/(m_mod² V∥) ≪ 1. The lattice symmetry that makes V″(0) vanish (Eq. 2.18) protects the inflaton's quartic flatness but does nothing for the volume modulus; this is the standard η problem of string inflation. The paper never checks whether a stabilization satisfying these inequalities exists, nor whether the required hierarchy is natural given M_s r⊥ ≫ 1 and M_p r⊥ ~ 10⁶. A concrete addition would be to state the required m_mod/H explicitly and to indicate whether any known stabilization mechanism (fluxes, wrapped branes) can supply it without spoiling the flatness of Eq. 2.19. If m_mod ≲ H, V∥ rolls during inflation, changing A and the canonical normalization ψ ∝ y√(T_p V∥) (Eq. 2.8), and the slow-roll analysis of Eqs. 2.19–2.23 does not apply.
[Introduction and §2.5] The Introduction states that the authors 'identify these special initial conditions explicitly for toroidal compactifications and show that they are sufficiently large for inflation not to be unlikely given a reasonable density of branes and antibranes in the extra dimensions.' §2.5 does not deliver this estimate. It gives z* ≈ 0.1 r⊥ (Eq. 2.22) and z_end ≈ 0.5 r⊥ and calls them 'fairly natural numbers,' but never computes the volume fraction of the slow-roll region in the d⊥-dimensional cell, nor converts that fraction into a probability given a brane density. For d⊥ = 6 the central region |z| < 0.5 r⊥ is a small fraction of the cell, so the claim is not obviously true and needs an explicit number. Please either supply the volume-fraction and probability estimate that the Introduction promises, or soften the Introduction to say that the special regions are identified but their statistical weight is left for future work.
[§2.5, Eqs. (2.20)–(2.24)] The coefficient γ in Eq. (2.20) is asserted to be 'a constant of order O(1)' but is never computed. Since δ_H in Eq. (2.21) depends on γ, the COBE normalization M_p r⊥ ≈ 1.3×10⁶ and hence the headline value r⊥⁻¹ ~ 10¹² GeV (Eq. 2.24) carry an unquantified O(1) uncertainty. This is a precision issue rather than a correctness issue — the order of magnitude survives if γ is genuinely O(1) — but Eq. (2.24) is the paper's one quantitative contact with observation, and the quartic lattice sum is a finite, doable calculation for the hypercubic torus (the paper already sketches the corresponding argument for the vanishing of the second derivative). Please compute γ explicitly, or state the uncertainty in Eq. (2.24) as a range rather than a single number.

Minor objections (7)

[§2.4] The dismissal of asymmetric compactification — 'this stratagem turns out to fail ... may be shown by a simple scaling argument—or by considerations of T-duality—to be modified in this case to V ∼ 1/(aⁿ y^{d⊥−n})' — is asserted rather than shown. Since this closes off an obvious escape route from the negative result, please display the derivation of the modified potential and the resulting bound y ≫ (V⊥ aⁿ)^{1/(d⊥−n)}.
[Abstract and §3, footnote 9] The abstract says the cascade 'naturally stops with the production of 3-branes in 10-dimensional string theory,' but footnote 9 concedes that in Type IIA the cascade would stop at 4-branes. Please qualify the abstract to Type IIB or Type I, where the D9–D9 starting point applies.
[End of §3] The sentence 'This is the first time that inflation is achieved from a computable potential in string theory' is stronger than the body supports: the potential is computable given the frozen-moduli assumption of §2.3 and up to the uncomputed coefficient γ of Eq. (2.20). Please qualify the priority claim accordingly.
[Footnote 6 and Ref. [11]] The disagreement with Dvali, Solganik and Shafi is stated in footnote 6, but Ref. [11] is listed as 'to appear,' so the reader cannot assess the point at issue. Please spell out the disagreement in a sentence or update the reference at publication.
[Eq. (2.21)] The intermediate steps from Eq. (2.19) to Eq. (2.21) are not shown. Since Eq. (2.24) is a headline number, please display the derivation of δ_H from the quartic potential so that the reader can verify the normalization.
[Fig. 1 caption] The caption notes that antibrane images are omitted because the antibrane–antibrane force vanishes, which is correct, but it would help to state explicitly that brane–brane images are included in the sum of Eq. (2.17) while antibrane images are not, to avoid confusion about what the lattice sum represents.
[Throughout] There are several typographical errors, including 'annilate' (p. 15), 'tunning' (p. 16), and 'supersymmetry is recovered guarantees' (p. 16). A table listing d⊥ = d − p + 3 (Eq. 2.4) for the cases discussed (d = 6, p = 3, 5, 9) would also help the reader follow which transverse dimension count applies where.

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The paper

The paper claims

Brane-antibrane motion near a symmetric point of a compact torus gives a quartic potential flat enough for 60 e-folds, with spectral index n-1 = -3/N and a compactification scale near 10^12 GeV.

The reading

The paper asks whether the force between a D-brane and an anti-D-brane, moving toward each other through the six extra dimensions of string theory, can drive inflation in the four dimensions we see. The inflaton is the distance between the two objects. The authors first show that the answer is no in the generic case: the string-theory force is too strong, so the pair falls together far too fast to give 60 e-folds of expansion. Equation 2.13 makes this quantitative, and the paper states the failure plainly rather than hiding it. This is the honest negative result that most of the paper's value rests on, and it is why the authors disagree with a contemporaneous preprint that reached the opposite conclusion (footnote 6). The rescue comes from geometry. If the extra dimensions form a torus and the anti-brane sits at the exact centre of a cell, the pull from the surrounding image branes cancels not only in force but also in the quadratic term of the potential. The leading term is then quartic, the potential is flat near the centre, and slow roll becomes possible for small displacements. The authors compute the resulting spectrum: the index is slightly below one, n-1 = -3/N, and matching the COBE amplitude fixes the compactification scale at about 10^12 GeV. Inflation ends when the separation shrinks to the string scale and a tachyon develops, reheating the universe in a stringy version of hybrid inflation. The final section argues, qualitatively, that repeated annihilations cascade down to three-branes and stop there.

Extended reading notes

Core claim

Near the centre of a hypercubic torus cell the brane-antibrane potential has vanishing first and second derivatives (Eq. 2.18), so the leading term is quartic, V = A - (1/4)Cz^4 (Eq. 2.19). This makes slow roll automatic for small displacements, giving eta = -3 gamma (z/r_perp)^2 (Eq. 2.21), a spectral index n-1 = -3/N (Eq. 2.23), and, after COBE normalization, M_p r_perp = 1.3 x 10^6, i.e. r_perp^-1 = 10^12 GeV (Eq. 2.24). If correct, this is a working inflationary model whose potential is computed from string theory rather than assumed.

Load-bearing premise

Section 2.3 opens by assuming that all compactification moduli, including the transverse volume V_perp, the parallel volume V_parallel, the dilaton and the shape of the torus, are frozen by 'some unknown physics' and can be treated as fixed parameters during inflation. Every subsequent equation, including the 4D reduction of Eq. 2.7, the canonical normalization of Eq. 2.8, and the flatness of V(y) in Eq. 2.19, depends on this. If the volume or shape moduli roll on the same timescale as the inter-brane separation, the effective 4D potential is not the one computed here and the slow-roll analysis does not apply.

Original abstract

We show how the motion through the extra dimensions of a gas of branes and antibranes can, under certain circumstances, produce an era of inflation as seen by observers trapped on a 3-brane, with the inflaton being the inter-brane separation. Although most of our discussion refers to arbitrary p-branes, when we need to be specific we assume that they are D-branes of Type II or Type I string theory. For realistic brane couplings, such as those arising in string theory, the inter-brane potentials are too steep to inflate the universe for acceptably long times. However, for special regions of the parameter space of brane-antibrane positions the brane motion is slow enough for there to be sufficient inflation. Inflation would be more generic in models where the inter-brane interactions are much weaker. The spectrum of primordial density fluctuations predicted has index n slightly less than 1, and an acceptable amplitude, provided that the extra dimensions have linear size 1/r ~ 10^{12} GeV. Reheating occurs as in hybrid inflation, with the tachyonic instability of the brane-antibrane system taking over for small separations. The tachyon field can induce a cascade mechanism within which higher-dimension branes annihilate into lower-dimension ones. We argue that such a cascade naturally stops with the production of 3-branes in 10-dimensional string theory.

The compiled record

The paper's own sentences, arranged, kept beside the review and separate from it. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

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What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.94 · human participants 0.01 · controlled comparison 0.02 · randomized assignment 0.01 · states quantitative result 0.95 · compares with prior results 0.16 · mentions code or data availability 0.01.

The abstract, sentence by sentence

arXiv listing abstract v3. Results and the main claim are underlined; show every role.

We show how the motion through the extra dimensions of a gas of branes and antibranes can, under certain circumstances, produce an era of inflation as seen by observers trapped on a 3-brane, with the inflaton being the inter-brane separation. Although most of our discussion refers to arbitrary p-branes, when we need to be specific we assume that they are D-branes of Type II or Type I string theory. For realistic brane couplings, such as those arising in string theory, the inter-brane potentials are too steep to inflate the universe for acceptably long times. However, for special regions of the parameter space of brane-antibrane positions the brane motion is slow enough for there to be sufficient inflation. Inflation would be more generic in models where the inter-brane interactions are much weaker. The spectrum of primordial density fluctuations predicted has index n slightly less than 1, and an acceptable amplitude, provided that the extra dimensions have linear size 1/r ~ 10^{12} GeV. Reheating occurs as in hybrid inflation, with the tachyonic instability of the brane-antibrane system taking over for small separations. The tachyon field can induce a cascade mechanism within which higher-dimension branes annihilate into lower-dimension ones. We argue that such a cascade naturally stops with the production of 3-branes in 10-dimensional string theory.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	We show how the motion through the extra dimensions of a gas of branes and antibranes can, under certain circumstances, produce an era of inflation as seen by observers trapped on a 3-brane, with the inflaton being the inter-brane separation.	contribution 0.85	0.92	0.82	asserted 0.86
s1	Although most of our discussion refers to arbitrary p-branes, when we need to be specific we assume that they are D-branes of Type II or Type I string theory.	method 0.59	0.26	0.03	asserted 0.85
s2	For realistic brane couplings, such as those arising in string theory, the inter-brane potentials are too steep to inflate the universe for acceptably long times.	limitation 0.81	0.51	0.09	asserted 1.00
s3	However, for special regions of the parameter space of brane-antibrane positions the brane motion is slow enough for there to be sufficient inflation.	result 0.78	0.72	0.16	asserted 0.71
s4	Inflation would be more generic in models where the inter-brane interactions are much weaker.	interpretation 0.68	0.32	0.08	hedged possibility 0.56
s5	The spectrum of primordial density fluctuations predicted has index n slightly less than 1, and an acceptable amplitude, provided that the extra dimensions have linear size 1/r ~ 10^{12} GeV.	result 1.00	0.84	0.12	asserted 0.85
s6	Reheating occurs as in hybrid inflation, with the tachyonic instability of the brane-antibrane system taking over for small separations.	result 0.88	0.66	0.05	asserted 1.00
s7	The tachyon field can induce a cascade mechanism within which higher-dimension branes annihilate into lower-dimension ones.	result 0.62	0.60	0.06	hedged possibility 0.52
s8	We argue that such a cascade naturally stops with the production of 3-branes in 10-dimensional string theory.	interpretation 0.55	0.63	0.14	hedged possibility 0.43

What kind of paper the classifier reports this is: theoretical result 1.00 · evidence from proof or derivation 0.61.

What was examined, and what was not

sources read

arXiv listing abstract v3

not examined

full text
figures and tables
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relations to other papers

levels run

P abstract

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Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

Figures

**Figure 1.** The covering space of a square torus. Solid circles represent images of the Dp brane, and the open circle represents the Dp brane, which is near the center of a hyper-cubic cell during the slow-roll inflationary phase. The images of the antibrane are omitted because they do not contribute to the potential of the antibrane since the force between an antibrane and another antibrane is zero. the center of the hyper-cubic cell at the time when the COBE perturbation leaves the horizon during the inflation is z∗ ≈ r⊥ √ 2 γ N . (2.22) From this the spectral index and its derivati

**Figure 2.** The figure on the left shows two branes along orthogonal directions of a long cylinder. In the middle, the branes reconnect. The final configuration, shown on the right, consists of a single brane winding once around the compact direction. universe with branes aligned with the large dimensions of space seems to be selected in such a natural way. Notice that our arguments are not identical to the one given in [21], but complements it in an interesting way. Their argument was based on the fact that winding modes tend to compactify the space dimensions where they are winding around

Figures reproduced from arXiv:hep-th/0105204 by the authors.

References

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Observational Signatures and Non-Gaussianities of General Single Field Inflation
hep-th 2006-05 accept novelty 6.0 of 10

For any single-field inflation model whose Lagrangian depends only on the inflaton and its first derivative, the full primordial three-point function at first order in slow variation is fixed by five parameters and de...
Warped Spectroscopy: Localization of Frozen Bulk Modes
hep-th 2006-03 conditional novelty 6.0 of 10

The lightest dilaton-axion KK mode in long warped throats localizes at the throat bottom with mass near the warped string scale, comparable to the KK gap.
Inflating in a Better Racetrack
hep-th 2006-03 conditional novelty 6.0 of 10

An explicit type IIB compactification with two Kahler moduli can support racetrack inflation driven by a linear combination of axions, matching the COBE spectrum with n_s approximately 0.95.
Kahler Moduli Inflation
hep-th 2005-09 conditional novelty 6.0 of 10

A blow-up Kähler modulus in large-volume type IIB flux compactifications supplies a naturally flat inflaton direction, giving n_s = 1 - 2/N_e between 0.960 and 0.967 with a tensor fraction below 10^-10.
String Loop Corrections to Kahler Potentials in Orientifolds
hep-th 2005-08 conditional novelty 6.0 of 10

One-loop string amplitudes give explicit corrections to the Kähler potential of type IIB orientifolds that depend on both closed and open string moduli.
A Circle That Won't Return: The Fate of RR Fluxes and D-branes in Type 0A Tachyon Condensation
hep-th 2026-06 unverdicted novelty 5.0 of 10

In type 0A on a two-circle wedge, isolated collapsing-branch D_p^- sources incur infinite RR field energy cost as the branch shrinks, with possible infrared screening or discharge to D_p^+ via an effective relative-ch...
Fibre Inflation Meets Quintessence: Implications of Perturbative Stabilisation
hep-th 2025-11 reject novelty 5.0 of 10

Adding a base-modulus redefinition to fibre inflation in perturbative LVS shifts (ns, r) into ACT-allowed territory and yields an axion quintessence companion.
The BAO-CMB Tension and Implications for Inflation
astro-ph.CO 2025-07 accept novelty 5.0 of 10

The upward shift in the scalar spectral index n_s in CMB+BAO analyses is driven by the combined effects of a known CMB degeneracy and the tension between CMB and DESI BAO data, not by new information about n_s itself.
Towards hybrid inflation with $n_s=1$ in light of Hubble tension and primordial gravitational waves
astro-ph.CO 2022-05 conditional novelty 5.0 of 10

Hybrid inflation ending in a waterfall instability can lift the scalar spectral index to ns = 1, reviving chaotic φ² inflation when combined with early dark energy.
Poly-instanton Inflation
hep-th 2011-10 conditional novelty 5.0 of 10

Poly-instanton corrections to the type IIB superpotential can drive slow-roll inflation on a Kähler fibre modulus, predicting ns about 0.96 and r about 10^-5.
Cosmic string loop distribution on all length scales and at any redshift
astro-ph.CO 2010-06 conditional novelty 5.0 of 10

Cosmic string loops settle into a universal scaling distribution on all length scales, with a scale-independent plateau below the gravitational backreaction cutoff, and today's loop density is bounded in terms of the ...
Running Non-Gaussianities in DBI Inflation
astro-ph 2005-07 conditional novelty 5.0 of 10

In the infrared DBI inflation model the equilateral non-Gaussianity is f_NL of order 0.036 beta-squared N_e-squared, within current bounds for beta of order one, and its logarithmic running traces the warp geometry.
Tachyonic Instability and Dynamics of Spontaneous Symmetry Breaking
hep-th 2001-06 accept novelty 5.0 of 10

Spontaneous symmetry breaking from a tachyonic (negative mass squared) potential completes within one oscillation of the field distribution, because the instability converts potential energy into colliding classical w...
Engineering a Digital Twin for the Monitoring and Control of Beer Fermentation Sampling
cs.SE 2025-08 unverdicted novelty 4.0 of 10

An experience report claims a Type 2 digital twin for beer fermentation reduces manual sampling time by 91% and enables control at seven bar.
Hybrid cosmological attractors
hep-th 2022-04 conditional novelty 4.0 of 10

Uplifting an α-attractor potential with a hybrid-inflation sector produces a second attractor with ns = 1, continuously interpolating to the standard 1 - 2/N as the uplift or critical field shrinks.
Magnetic monopoles revisited: Models and searches at colliders and in the Cosmos
hep-ph 2020-05 accept novelty 3.0 of 10

Several Standard-Model extensions admit finite-energy magnetic monopoles with masses of a few TeV, and LHC searches now exclude them up to roughly 2.1 to 3.75 TeV depending on magnetic charge and spin.
String Inflation After Planck 2013
hep-th 2013-06 conditional novelty 3.0 of 10

A survey of string-inflation models finds that their pre-Planck predictions mostly sit near the observed spectral index with very small tensor-to-scalar ratio, so future tensor detection would rule out most of them.
String Cosmology: A Review
hep-th 2007-10 accept novelty 3.0 of 10

String cosmology's central obstacle is the eta problem: moduli stabilization generically generates inflaton mass terms of order the Hubble scale, and no fully explicit, correction-controlled string inflation model yet exists.
Brane Inflation : String Theory viewed from the Cosmos
hep-th 2006-10 conditional novelty 3.0 of 10

Brane inflation in a warped flux compactification generically produces enough e-folds and leaves a scaling network of cosmic superstrings with tension between 10^-13 and 10^-6, testable by CMB, lensing, and gravitatio...
Toward Realistic Intersecting D-Brane Models
hep-th 2005-01 accept novelty 3.0 of 10

A structured survey of intersecting D-brane model building: how gauge groups, chiral families, Yukawa couplings and soft terms arise from D-branes wrapping intersecting cycles, and why no fully realistic model exists yet.
Introduction to Cosmic F- and D-Strings
hep-th 2004-12 accept novelty 3.0 of 10

Cosmic-scale F- and D-strings can arise naturally when branes annihilate at the end of warped brane inflation, and their gravitational-wave cusps could be detectable by LIGO.
Remarks on brane-antibrane inflation
hep-th 2025-01 conditional novelty 2.0 of 10

The paper reviews how a perfect-square structure in the scalar potential can stabilize the volume modulus and evade the eta problem in brane-antibrane inflation.
Moduli Stabilization in String Theory
hep-th 2023-10 accept novelty 2.0 of 10

This is a review of moduli stabilization in string compactifications, organizing the KKLT and Large Volume Scenario constructions, their extensions to other string theories, and their cosmological and particle-physics...
String moduli inflation: an overview
hep-th 2011-08 accept novelty 2.0 of 10

Most closed-string moduli inflation models surveyed here predict negligible gravitational waves, so a Planck detection of tensor modes would rule them out.
Seeking String Theory in the Cosmos
hep-th 2011-05 accept novelty 2.0 of 10

Cosmic superstrings can form and survive in brane-inflation models, and existing CMB, pulsar-timing, lensing and cosmic-ray data already bound their tension at roughly G mu < 6e-7, with suppressed intercommutation as ...
Tachyon Dynamics in Open String Theory
hep-th 2004-10 accept novelty 2.0 of 10

A comprehensive review of open string tachyon condensation argues that unstable D-brane dynamics is captured by an internally consistent open string field theory without explicit closed-string coupling.
Lectures on Naturalness, String Landscape and Multiverse
hep-th 2020-08 unverdicted novelty 1.0 of 10

Lecture notes providing a technical introduction to naturalness problems and the string theory landscape for graduate students.

How the literature uses it

93 arXiv papers cite this in 137 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 58 sentences without a confident label

Contests it 1 paper

In this way we managed to avoid the $η$-problem and derived for the first time the inverse power-law potential originally proposed in [ref] , instead of the tuned inflection point inflation model of [ref] that is now in conflict with observations.

Back to the origins of brane-antibrane inflation · Conclusions · contest 0.81

Compares with it 2 papers

As it turns out, this realisation of D3/D7 inflation suffers from a similar problem as the brane-antibrane proposal [ref] , i.e. the potential is too steep.

Fluxbranes: Moduli Stabilisation and Inflation · Introduction · 0.93
In the opposite regime to Eq. [ref], i.e., [equation] during inflation, the kinetic coefficient of Eq. [ref] is approximated as constant, and the canonically normalized field $ψ$ is given by [equation] In the same way as the previous calculation, we can obtain the relation between the e-folding $N$ and the field value $ψ$ or $τ_2$, [equation] for $τ_2 ≫1$, and based on this, the inflationary observable $(n_s,r)$ are estimated as [equation] The CMB normalization fixes $V_0$ as [equation] Note that the potential form in Case II, $V_J(ψ) ∼(1-𝒞/ψ)^2$, with a constant $𝒞$, and hence its observational predictions [ref] and [ref] resemble those of the brane inflation scenario [ref] .

Higgs-Modular Inflation · Case II (Higgs-like) · 0.93

Cites it as support 1 paper

However it is impossible to separate them by more than the size of the extra dimensions, so this does not work [ref] .

Fine-Tuning in Brane-antibrane Inflation · The flatness problem · 0.97

Cites it as background 66 papers

In this paper, we will focus on one of the most well developed inflationary scenarios in string theory, i.e. $D$ brane inflation [ref] (see also Refs. [ref] ; for reviews, see Ref. [ref] and references therein), where the inflaton field is identified with the position of a space-filling mobile $D$ brane, usually a $D3$ brane, in a warped six dimensional manifold [ref] .

Systematics of multi-field effects at the end of warped brane inflation · Introduction · 0.94
Historically, following the seminal paper [ref] , the first example of an inverse power-law potential in string cosmology has been actually proposed in the original formulation of brane-antibrane inflation which features $n=4$ [ref] .

Back to the origins of brane-antibrane inflation · Introduction · 0.90
Brane-antibrane inflation [ref] is a particularly sharp example: unlike ordinary single-field models, where reheating is usually modeled by perturbative inflaton decay, D3/$D3$ inflation ends when the open string stretched between the brane and antibrane becomes tachyonic [ref] and the pair annihilates.

Fire at the Tip of the Throat: Hagedorn Phase after brane-antibrane inflation? · Introduction · 0.98

Discussion

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