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An A star on an M star during a flare within a flare

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Paper breakdownThe authors' claims, conditions and measurements, as JSON Signed receiptProof this review has not been altered
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Adam F. Kowalski (1), Suzanne L. Hawley (1), Jon A. Holtzman (2), John P. Wisniewski (1), Eric J. Hilton (1) ((1) University of Washington, (2) New Mexico State University)

Solar and Stellar Astrophysics · Submitted 3 Oct 2010

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim The amount of heating implied by our model (\Delta T_phot ~ 16,000K) is far more than predicted by chromospheric backwarming in current 1D RHD flare models (\Delta T_phot ~ 1200K).

how it is stated · asserted 1.00 read the record →

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arXiv ID1010.0452 (version 1)
Pith ID5AXDNLTC, Pith's permanent record of this paper and its review
Citation(2) New Mexico State University), Adam F. Kowalski (1), Eric J. Hilton (1) ((1) University of Washington, John P. Wisniewski (1), Jon A. Holtzman (2), Suzanne L. Hawley (1). "An A star on an M star during a flare within a flare." arXiv:1010.0452 (2010). https://pith.science/paper/5AXDNLTC
Claim paper

The compiled record

The paper's own sentences, arranged. 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.

Open the compiled record

Compiled by classifier-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 4,321 input tokens, $0.0002 reported.

What the abstract itself states, as probabilities: claims first 0.07 · states limitation 0.52 · human participants 0.01 · controlled comparison 0.10 · randomized assignment 0.01 · states quantitative result 0.98 · compares with prior results 0.93 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v1. Results and the main claim are underlined; .

M dwarfs produce explosive flare emission in the near-UV and optical continuum, and the mechanism responsible for this phenomenon is not well-understood. We present a near-UV/optical flare spectrum from the rise phase of a secondary flare, which occurred during the decay of a much larger flare. The newly formed flare emission resembles the spectrum of an early-type star, with the Balmer lines and continuum in absorption. We model this observation phenomonologically as a temperature bump (hot spot) near the photosphere of the M dwarf. The amount of heating implied by our model (\Delta T_phot ~ 16,000K) is far more than predicted by chromospheric backwarming in current 1D RHD flare models (\Delta T_phot ~ 1200K).

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#sentencerolethe authors' own workstates the main conclusionstrength
s0 M dwarfs produce explosive flare emission in the near-UV and optical continuum, and the mechanism responsible for this phenomenon is not well-understood. background 0.75 0.05 0.03 asserted 0.99
s1 We present a near-UV/optical flare spectrum from the rise phase of a secondary flare, which occurred during the decay of a much larger flare. contribution 0.93 0.96 0.07 asserted 1.00
s2 The newly formed flare emission resembles the spectrum of an early-type star, with the Balmer lines and continuum in absorption. result 1.00 0.89 0.15 asserted 0.99
s3 We model this observation phenomonologically as a temperature bump (hot spot) near the photosphere of the M dwarf. method 0.74 0.92 0.13 asserted 0.74
s4 The amount of heating implied by our model (\Delta T_phot ~ 16,000K) is far more than predicted by chromospheric backwarming in current 1D RHD flare models (\Delta T_phot ~ 1200K). result 0.68 0.74 0.65 asserted 1.00

What kind of paper the classifier reports this is: empirical study 1.00 · evidence from observation or experiment 0.99.

What was examined, and what was not

sources read
  • arXiv listing abstract v1
not examined
  • full text
  • figures and tables
  • references and citing sentences
  • relations to other papers
levels run
  • P abstract
not run
  • S sections
  • T body sentences
  • C citations
  • R cross-paper relations

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

The paper
Original abstract

M dwarfs produce explosive flare emission in the near-UV and optical continuum, and the mechanism responsible for this phenomenon is not well-understood. We present a near-UV/optical flare spectrum from the rise phase of a secondary flare, which occurred during the decay of a much larger flare. The newly formed flare emission resembles the spectrum of an early-type star, with the Balmer lines and continuum in absorption. We model this observation phenomonologically as a temperature bump (hot spot) near the photosphere of the M dwarf. The amount of heating implied by our model (\Delta T_phot ~ 16,000K) is far more than predicted by chromospheric backwarming in current 1D RHD flare models (\Delta T_phot ~ 1200K).

Human review

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How the literature uses it

1 arXiv paper cite this in 1 sentence

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

Compares with it 1 paper
  • On the other hand, another highly active dM4.5e star, YZ CMi, also exhibited a series of secondary flares during a white light mega-flare as described by [ref] , who also speculated that the flare on YZ CMi originated in a complex arcade with a sequence of reconnecting loops.

    Multi-wavelength observations of Proxima Centauri · Summary and conclusions · 0.89

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