{"arxiv_id":"astro-ph/0403315","incoming":{"papers":40,"sentences":53,"groups":[{"kind":"extends","label":"Builds on it","papers":2,"sentences":2,"quotes":[{"arxiv_id":"0805.4265","title":"Primordial statistical anisotropy generated at the end of inflation","url":"/paper/0805.4265","section":"Introduction","sentence":"This model is based on Ref [ref] , in which the authors consider the modified hybrid inflation adding a light scalar field other than inflaton in order to generate the large non-Gaussianity of primordial curvature perturbations.","intent_p":0.83,"contests_p":null},{"arxiv_id":"0710.2540","title":"Modulated Perturbations from Instant Preheating after new Ekpyrosis","url":"/paper/0710.2540","section":"Modulated Perturbations from Instant Preheating after Ekpyrosis","sentence":"That way we can provide a new realization of modulated perturbations from reheating [ref] ; the decay rate of $χ$-particles depends on this coupling and the radion field value via $Γ∝h^2 ϕ$ [ref] .","intent_p":0.8,"contests_p":null}]},{"kind":"background","label":"Cites it as background","papers":22,"sentences":22,"quotes":[{"arxiv_id":"1506.01469","title":"Constraints on variations in inflaton decay rate from modulated preheating","url":"/paper/1506.01469","section":"Introduction","sentence":"But there is an equally possible theory of generating density perturbations via variations in the decay rate of inflaton field after the end of inflation [ref] .","intent_p":0.83,"contests_p":null},{"arxiv_id":"0806.4065","title":"Modulated Inflation (@SUSY08)","url":"/paper/0806.4065","section":"Introduction","sentence":"Another idea for the cosmological perturbation is “at the end” scenario [ref] [See the second picture in Fig.[ref].].","intent_p":0.87,"contests_p":null},{"arxiv_id":"0904.0793","title":"Preheating and the non-gaussianity of the curvature perturbation","url":"/paper/0904.0793","section":"The non-inflaton contribution","sentence":"Possibilities in chronological order include generation (i) during multi-field inflation [ref] , (ii) at the end of inflation [ref] , (iii) during preheating as we discussed in the Introduction, (iv) during modulated reheating [ref] , (v) at a modulated phase transition [ref] and (vi) before a second reheating through the curvaton mechanism [ref] .","intent_p":0.95,"contests_p":null},{"arxiv_id":"0810.3291","title":"Non-standard kinetic term as a natural source of non-Gaussianity","url":"/paper/0810.3291","section":"Introduction","sentence":"For example, generation of non-Gaussian perturbations may occur (1) during inflation by a step-like potential [ref] , (2) during inflation by a kinetic term [ref] , (3) during inflation by a modulated velocity [ref] , (4) at the end of inflation [ref] , (5) after inflation at (p)reheating [ref] , and (6) long after inflation [ref] .","intent_p":0.88,"contests_p":null},{"arxiv_id":"0902.4283","title":"Cosmological perturbations from an inhomogeneous phase transition","url":"/paper/0902.4283","section":"Introduction","sentence":"Another way to generate cosmological perturbations from an inhomogeneous boundary is to consider an inhomogeneous end for the inflationary phase [ref] .","intent_p":0.82,"contests_p":null}]}],"unlabelled_sentences":29},"outgoing":{"papers":0,"sentences":0,"groups":[],"unlabelled_sentences":0},"claims":[],"thresholds":{"intent_p":0.8,"supports_p":0.95,"contests_p":0.7},"method":"Citing sentences come from each paper's LaTeX source; every \\cite marks the sentence and the works it cites. Pith's classifier typed each sentence. A label is shown at intent probability 0.8 or more (0.95 for support), a contest at 0.7 or more. Measured accuracy against two blind model families is at https://pith.science/accuracy. The quoted sentences are the citing authors' own.","held_up":null,"_links":{"html":"https://pith.science/paper/astro-ph/0403315"}}