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Theoretical constraints on brane inflation and cosmic superstring radiation
High Energy Physics - Theory · Submitted 9 May 2011
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We argue that in a warped background where one might expect axionic radiation to be enhanced relative to gravitational radiation, neithe F-strings nor D-strings can emit axionic radiation, while FD-strings cannot give rise to Neveu-Schwarz--Neveu-Schwarz particle emission, and their Ramond-Ramond particle emission is not well-defined.
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The abstract, sentence by sentence
We analyze theoretical constraints on the consistency of brane inflation leading to cosmic superstring formation and on the subsequent radiation of these cosmic superstrings. We first investigate the implications of recently elucidated supergravity constraints on models of brane inflation. We show that both D3/D7 and D3/anti-D3 brane inflation are subject to non-trivial constraints. Both models can be shown to satisfy those constraints, but for the case of D3/D7 there may be important consequences for the inflationary mechanism. We then analyze the strong theoretical constraints on the types of allowed radiation by cosmic superstrings, should they be formed; such constraints do not apply to their field theoretical analogues. We argue that in a warped background where one might expect axionic radiation to be enhanced relative to gravitational radiation, neithe F-strings nor D-strings can emit axionic radiation, while FD-strings cannot give rise to Neveu-Schwarz--Neveu-Schwarz particle emission, and their Ramond-Ramond particle emission is not well-defined.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We analyze theoretical constraints on the consistency of brane inflation leading to cosmic superstring formation and on the subsequent radiation of these cosmic superstrings. | contribution 0.97 | 0.87 | 0.10 | asserted 0.63 |
| s1 | We first investigate the implications of recently elucidated supergravity constraints on models of brane inflation. | contribution 0.77 | 0.73 | 0.03 | asserted 0.56 |
| s2 | We show that both D3/D7 and D3/anti-D3 brane inflation are subject to non-trivial constraints. | result 0.98 | 0.86 | 0.12 | asserted 1.00 |
| s3 | Both models can be shown to satisfy those constraints, but for the case of D3/D7 there may be important consequences for the inflationary mechanism. | result 0.77 | 0.86 | 0.11 | hedged possibility 0.81 |
| s4 | We then analyze the strong theoretical constraints on the types of allowed radiation by cosmic superstrings, should they be formed; such constraints do not apply to their field theoretical analogues. | contribution 0.98 | 0.81 | 0.16 | asserted 0.98 |
| s5 | We argue that in a warped background where one might expect axionic radiation to be enhanced relative to gravitational radiation, neithe F-strings nor D-strings can emit axionic radiation, while FD-strings cannot give rise to Neveu-Schwarz--Neveu-Schwarz particle emission, and their Ramond-Ramond particle emission is not well-defined. | result 0.99 | 0.78 | 0.33 | asserted 0.81 |
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The paper
Original abstract
We analyze theoretical constraints on the consistency of brane inflation leading to cosmic superstring formation and on the subsequent radiation of these cosmic superstrings. We first investigate the implications of recently elucidated supergravity constraints on models of brane inflation. We show that both D3/D7 and D3/anti-D3 brane inflation are subject to non-trivial constraints. Both models can be shown to satisfy those constraints, but for the case of D3/D7 there may be important consequences for the inflationary mechanism. We then analyze the strong theoretical constraints on the types of allowed radiation by cosmic superstrings, should they be formed; such constraints do not apply to their field theoretical analogues. We argue that in a warped background where one might expect axionic radiation to be enhanced relative to gravitational radiation, neithe F-strings nor D-strings can emit axionic radiation, while FD-strings cannot give rise to Neveu-Schwarz--Neveu-Schwarz particle emission, and their Ramond-Ramond particle emission is not well-defined.
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How the literature uses it
7 arXiv papers cite this in 9 sentences
Papers citing it · 7 sentences without a confident label
Cites it as background 2 papers
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Within IIB string theory there are two classes of brane inflation models: D3/D7 inflation [ref] [It is worth noting the caveat discussed in Ref. [ref] .] and brane-antibrane inflation with D3/$D3$ [ref] being the most studied example.
How well do we understand the thermal history of the Universe? Implications of the recent BICEP2 data · Introduction · 0.86
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We wish to clarify whether a field-dependent FI term can play the role of an effective constant which drives inflation.[For alternative and recent attempts to reconcile inflation with field-dependent FI terms, see [ref] .] In the case of DHI we discuss a series of obstacles which prevent possible setups from resembling the simple controllable model introduced in [ref] .
Inflation with Fayet-Iliopoulos Terms · Introduction · 0.88
What it cites · 67 sentences without a confident label
Contests 1 paper
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However, taking the details of the string compactification into account leads to difficulties with the argument in Ref. [ref] .
Energy Radiation by Cosmic Superstrings in Brane Inflation · Allowed radiation from cosmic superstrings in a throat · contest 0.80
Compares with 1 paper
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It appears in the ten-dimensional (Einstein-frame) action as follows [The IIB action can also be given in $SL(2, ℤ)$ invariant form in terms of $G_3 = F_3 - τH_3$ where $τ= C_0 + ie^-ϕ$, but we consider the D- and F-string cases separately here.]: [equation] where $H = dB$ and the $S_local$ part of the action is given by [equation] Following Ref. [ref] we compare the four-dimensional action to that in Ref. [ref] , finding (we have to take $B_2 →B̃_2 = (M_P/2) √(β/g_s) B_2$): [equation] Then from Eqs. ([ref]) and ([ref]), the ratio $P_NS/P_g$ goes like $g_s^3$: [equation] so this radiation is suppressed compared to the RR particle radiation.
Energy Radiation by Cosmic Superstrings in Brane Inflation · NS particle emission · 0.83
Cites as support 2 papers
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Specifically, the volume of the K3 cannot be stabilized above the SUSY-breaking scale in a consistent way [ref] .
Comments on Supercurrent Multiplets, Supersymmetric Field Theories and Supergravity · D3/D7 inflation · 0.98
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As a result, at reheating almost all of the energy goes to the U(1) gauge bosons rather than into the Standard Model fields [ref] .]
Cosmic Strings and Superstrings · D3/$D3$ inflation · 0.97
Cites as background 17 papers
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Cosmic superstrings, produced at the end of brane inflation [ref] , can be F-strings (the fundamental strings of string theory), D-strings (one-dimensional Dirichlet branes) or $(p,q)$ strings, which are bound states of $p$ F-strings and $q$ D-strings.
Cosmic String Production Towards the End of Brane Inflation · Cosmic superstrings · 0.99
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[We refer the reader to, for example, Refs. [ref] for a detailed explanation of the orientifold action.] The action of $O$ on the NS-NS and RR two-forms is [equation] respectively.
The effective action of N=1 Calabi-Yau orientifolds · Constraints from the orientifold projection · 0.98
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[We refer the reader to, for example, Refs. [ref] for a detailed explanation of the orientifold action.] The action of $O$ on the NS-NS and RR two-forms is [equation] respectively.
String Loop Moduli Stabilisation and Cosmology in IIB Flux Compactifications · Constraints from the orientifold projection · 0.98
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