pith. sign in

arxiv: 2605.19571 · v1 · pith:MAW35TU6new · submitted 2026-05-19 · 🌌 astro-ph.HE

From mass-loss histories to lightcurves: a generalised framework for interaction-powered transients

Nikhil Sarin , Ryosuke Hirai This is my paper

Pith reviewed 2026-05-20 04:27 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords interaction-powered transientscircumstellar materialthin-shell approximationsupernova lightcurvesmass-loss historymulti-wavelength modelingType IIn supernovae
0
0 comments X p. Extension
pith:MAW35TU6 Add to your LaTeX paper What is a Pith Number? 
\usepackage{pith}
\pithnumber{MAW35TU6}

Prints a linked pith:MAW35TU6 badge after your title and writes the identifier into PDF metadata. Compiles on arXiv with no extra files. Learn more

The pith

A fast framework solves thin-shell dynamics to model lightcurves from ejecta colliding with arbitrary circumstellar material.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper introduces a computational method that solves the thin-shell equations of motion for supernova ejecta interacting with circumstellar material having any density or velocity profile. It provides two ways to turn the shock power into optical lightcurves and can also predict radio and X-ray emission from the same solution. A sympathetic reader would care because the method runs in milliseconds, supports complex time-variable mass loss, and reproduces the main results of far more expensive radiation-hydrodynamics runs, making it practical to analyze the growing sample of observed interacting transients.

Core claim

We introduce a fast generalised framework that solves the thin-shell equations of motion for ejecta colliding with circumstellar material of arbitrary density and velocity profiles. For optical and UV lightcurves the framework offers a one-zone mode based on instantaneous shock power and a finite-shell transport mode that follows trapped radiation, diffusion, shock emergence and post-emergence cooling. The same shock solution is used to generate radio synchrotron and thermal bremsstrahlung X-ray predictions. Benchmark tests show that the transport calculation together with a time-dependent shock-efficiency prescription recovers the main qualitative and quantitative features of a one-zone one

What carries the argument

The thin-shell equations of motion for ejecta colliding with circumstellar material, solved numerically to obtain the time-dependent shock radius, velocity and power for arbitrary CSM profiles.

If this is right

  • Inferred mass-loss parameters change noticeably when the assumed circumstellar velocity profile is altered even if the density at explosion is held fixed.
  • Aspherical circumstellar material can produce bolometric lightcurves that closely resemble those expected from multiple spherical shells.
  • The framework can recover a synthetic time-variable mass-loss history from mock observations.
  • Self-consistent optical, radio and X-ray predictions become available from a single shock solution.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The speed of the method opens the possibility of fitting large statistical samples of transients to map the diversity of pre-explosion mass-loss episodes across supernova types.
  • Extending the transport module to include wavelength-dependent opacities could improve predictions for ultraviolet and infrared bands without sacrificing the overall speed.
  • The ability to treat aspherical geometries suggests a route to testing whether many apparently multi-shell events are actually single asymmetric outflows viewed at different angles.

Load-bearing premise

The thin-shell approximation plus one-zone or finite-shell transport is accurate enough to capture the dynamics and radiation output even when the circumstellar material has complicated, time-variable structure.

What would settle it

A side-by-side comparison of the framework's bolometric lightcurve and spectral evolution against a full radiation-hydrodynamics simulation for a supernova with a highly structured, time-variable circumstellar shell would show whether the approximations remain valid or diverge.

Figures

Figures reproduced from arXiv: 2605.19571 by Nikhil Sarin, Ryosuke Hirai.

Figure 1
Figure 1. Figure 1: Static finite power-law CSM benchmark for the transport solver. The CSM is a finite shell with 𝑀CSM = 1 M⊙ and 𝑅in = 5 × 102 R⊙. The left panel shows a compact shell with 𝑅out = 5 × 103 R⊙, while the right panel shows an extended shell with 𝑅out = 5 × 104 R⊙. In both panels the CSM density follows 𝜌csm ∝ 𝑟 −𝑠 , with 𝑠 = 0, 0.5, 1, 1.5, and 2. The ejecta are a broken power-law supernova model with 𝑀ej = 5 M… view at source ↗
Figure 2
Figure 2. Figure 2: Comparison between our semi-analytic luminosity treatments and a one-dimensional radiation-hydrodynamical lightcurve for the same compact CSM configuration. The red curve shows the raw thin-shell shock power be￾fore photon diffusion or efficiency losses. The orange and purple curves show the one-zone luminosity with constant 𝜖 = 1 and with the time-dependent 𝜖 (𝑡) prescription, respectively. The green and … view at source ↗
Figure 3
Figure 3. Figure 3: Overview of CSM interaction model capabilities demonstrating the diversity of observable signatures from different mass-loss scenarios.Top left: Three representative mass-loss histories: a constant stellar wind at 𝑀¤ = 10−5 M⊙ yr−1 , a Gaussian outburst peaking 50 yr before explosion with 𝑀¤ peak = 10−4 M⊙ yr−1 , and a smooth triple power-law mass-loss history with breaks at 5 and 50 yr. Top right: Corresp… view at source ↗
Figure 4
Figure 4. Figure 4: Multi-eruption CSM scenarios demonstrating the diversity of interaction signatures from complex pre-supernova mass-loss histories. Left: Circum￾stellar density profiles for three representative scenarios: a single smooth eruption (blue), two eruptions producing one additional dense shell (green), and a three-eruption sequence producing multiple density enhancements (purple). The blue model uses a single ex… view at source ↗
Figure 5
Figure 5. Figure 5 [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Bolometric lightcurve for a SN with aspherical CSM. We model both the CSM and SN ejecta as explosions with broken power-law density distributions (𝛿 = 0.5, 𝑛 = 12). The equatorial density distribution is equiva￾lent to 𝑀exp = 1 M⊙ and 𝐸exp = 1049 erg, while the polar density distribution is equivalent to 𝑀exp = 0.2 M⊙ and 𝐸exp = 1049 erg. We assume a polar half￾opening angle of 70 deg and combine the indep… view at source ↗
Figure 7
Figure 7. Figure 7: Physical properties and LSST photometry for the representative multi-eruption CSM scenarios. Top left: Shell velocity evolution, showing the deceleration and re-acceleration caused by different CSM density structures. Top right: Raw shock luminosity before conversion to broadband magnitudes. Bottom panels: Synthetic LSST photometry in 𝑢 (solid), 𝑟 (dashed), and 𝑦 (dotted) bands at redshift 𝑧 = 0.001, assum… view at source ↗
Figure 8
Figure 8. Figure 8: Self-consistent radio and X-ray diagnostics for four representative CSM scenarios. The left panel shows 5 GHz synchrotron spectral luminosities, 𝐿𝜈, while the right panel shows intrinsic 0.3–10 keV thermal bremsstrahlung (free-free) luminosities. The four curves correspond to a constant wind (blue; 𝑀¤ = 10−4 M⊙ yr−1 , 𝑣𝑤 = 500 km s−1 ), a Gaussian outburst in the mass-loss history (green; baseline 𝑀¤ = 10−… view at source ↗
Figure 9
Figure 9. Figure 9: Top: Posterior predictive lightcurve for the Gaussian wind inference test. Data points show synthetic observations with 12% fractional uncertainty. The red line shows the true model and the blue shaded region the 95% posterior credible interval. Bottom: Recovered mass-loss history. The red line shows the true Gaussian wind profile and blue shaded regions the 95% posterior credible interval. Despite signifi… view at source ↗
Figure 10
Figure 10. Figure 10: Bolometric luminosity data and our fits to the lightcurve for all six real transients analysed in this work. The blue bands show the 90% credible interval. The lower panel in each object shows (𝐿data − 𝐿model)/𝜎 relative to the maximum-likelihood curve, using the same uncertainties as the likelihood. The x-axis is shown as rest-frame time in days; the zero point follows the convention of the underlying bo… view at source ↗
Figure 11
Figure 11. Figure 11: Inferred mass-loss histories or density profiles at the time of the supernova (90% credible interval based on the lightcurve fits) for all six real transients analysed in this work. MNRAS 000, 1–22 (2026) [PITH_FULL_IMAGE:figures/full_fig_p016_11.png] view at source ↗
read the original abstract

We introduce a fast ($\sim 1$-$50$ ms) and generalised framework for modelling interaction-powered transients. The framework solves the thin-shell equations of motion for ejecta colliding with circumstellar material (CSM), and supports arbitrary CSM density and velocity profiles, including steady winds, eruptions, and complex time-variable mass-loss histories. For optical/UV lightcurves, we implement two luminosity treatments: a fast one-zone mode based on the thin-shell shock power, and a finite-shell transport mode that evolves trapped radiation, photon diffusion, shock emergence, and post-emergence cooling for finite, static CSM shells. In a benchmark comparison, the transport calculation and an optional time-dependent shock-efficiency prescription reproduce the main qualitative and quantitative features of a one-dimensional radiation-hydrodynamical simulation. We use the same shock solution to post-process radio synchrotron and thermal bremsstrahlung X-ray predictions, enabling self-consistent multi-wavelength diagnostics. We show that the assumed CSM velocity structure can significantly affect inferred parameters even when the density profile at explosion is identical, and that aspherical CSM can mimic multiple spherical shells in bolometric lightcurves. We demonstrate the framework through recovery of a synthetic time-variable mass-loss history and applications to six transients: the Type IIn SN~2010jl, the rapidly evolving stripped-envelope SN~2023xgo, the Type Ia-CSM SN~2020aeuh, the hydrogen-poor superluminous SN~2015bn, the eruptive LBV-like transient SN~2009ip, and the long-duration interacting event iPTF14hls. The inferred CSM structures span steady or enhanced winds, thermonuclear interaction, eruptive density enhancements, and highly structured pre-supernova mass loss, illustrating the framework's utility for inference on upcoming large samples of interacting transients.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 3 minor

Summary. The manuscript introduces a fast (~1-50 ms) numerical framework for modeling interaction-powered transients. It solves the thin-shell equations of motion for ejecta colliding with circumstellar material (CSM) supporting arbitrary density and velocity profiles (steady winds, eruptions, time-variable mass loss). Luminosity is computed via a one-zone shock-power mode or a finite-shell transport mode that includes diffusion, emergence, and cooling. The transport calculation plus an optional time-dependent shock-efficiency prescription is benchmarked against a single 1D radiation-hydrodynamical simulation. The same shock solution is used for radio synchrotron and X-ray bremsstrahlung predictions. The framework is applied to recover a synthetic time-variable mass-loss history and to six observed transients (SN 2010jl, SN 2023xgo, SN 2020aeuh, SN 2015bn, SN 2009ip, iPTF14hls), with additional exploration of CSM velocity structure and asphericity effects on light curves.

Significance. If validated more broadly, the framework would offer a practical, computationally efficient tool for inferring mass-loss histories from the growing sample of interaction-powered transients. The support for arbitrary CSM profiles, self-consistent multi-wavelength outputs, and direct applications to real events are strengths that could facilitate population studies ahead of large surveys. The benchmark against RHD and the demonstration that velocity structure affects inferred parameters even at fixed density are useful contributions.

major comments (1)
  1. [Benchmark comparison section] § Benchmark comparison (and abstract): The central generality claim for arbitrary CSM profiles (including complex time-variable mass loss) rests on the thin-shell approximation plus one-zone/finite-shell transport reproducing RHD results. Only a single benchmark comparison is described; while it reproduces main qualitative and quantitative features, this is insufficient to establish robustness for highly structured or rapidly varying CSM where the instantaneous momentum balance of the thin-shell equations may miss multi-shock formation or radiative-precursor effects. Additional benchmarks with at least one structured-CSM case, together with quantitative metrics (e.g., luminosity residuals or energy conservation errors), are needed to support the claim.
minor comments (3)
  1. [Abstract] Abstract: The statement that the transport calculation 'reproduces the main qualitative and quantitative features' would be strengthened by citing the specific figure or table that shows the comparison and by reporting at least one numerical agreement metric.
  2. [Applications section] Applications section: When presenting the recovery of the synthetic time-variable mass-loss history, include a direct overlay or residual plot of the input versus recovered density profile to allow readers to assess the fidelity of the inference.
  3. [Methods section] Notation: The distinction between the one-zone and finite-shell transport modes is clear in the text, but a short summary table listing the assumptions, computational cost, and applicable regimes for each mode would improve readability.

Simulated Author's Rebuttal

1 responses · 1 unresolved

We thank the referee for their constructive review and for highlighting the importance of robust validation for the framework's generality claims. We address the major comment below and outline the revisions we will make to strengthen the manuscript.

read point-by-point responses

  1. Referee: [Benchmark comparison section] § Benchmark comparison (and abstract): The central generality claim for arbitrary CSM profiles (including complex time-variable mass loss) rests on the thin-shell approximation plus one-zone/finite-shell transport reproducing RHD results. Only a single benchmark comparison is described; while it reproduces main qualitative and quantitative features, this is insufficient to establish robustness for highly structured or rapidly varying CSM where the instantaneous momentum balance of the thin-shell equations may miss multi-shock formation or radiative-precursor effects. Additional benchmarks with at least one structured-CSM case, together with quantitative metrics (e.g., luminosity residuals or energy conservation errors), are needed to support the claim.

    Authors: We agree that a single benchmark limits the strength of the generality claim, particularly for highly structured or rapidly varying CSM where the thin-shell approximation may not capture multi-shock or radiative-precursor physics. We will revise the benchmark section to include quantitative metrics (luminosity residuals, energy conservation errors, and peak-time/peak-luminosity differences) for the existing comparison. We will also expand the discussion to explicitly note the limitations of the thin-shell approach for complex CSM and the conditions under which multi-shock effects could become important. However, generating additional radiation-hydrodynamical simulations for structured-CSM cases is computationally expensive and requires resources beyond those available for this revision; we therefore cannot add a new benchmark simulation at this time. The revised text will clarify that the current validation supports the framework's utility for the demonstrated applications while highlighting the approximation's scope. revision: partial

standing simulated objections not resolved
  • Performing additional radiation-hydrodynamical simulations for structured-CSM benchmark cases

Circularity Check

0 steps flagged

No significant circularity in derivation chain

full rationale

The paper introduces a numerical framework solving the standard thin-shell equations of motion for ejecta-CSM interaction with support for arbitrary density and velocity profiles. Luminosity is computed via one-zone shock power or finite-shell transport modes that evolve diffusion, emergence, and cooling. The benchmark comparison to an independent one-dimensional radiation-hydrodynamical simulation provides external validation rather than a self-referential reduction. No load-bearing step equates a prediction to a fitted input by construction, relies on self-citation chains for uniqueness, or renames known results as new derivations. The framework remains self-contained against the cited external benchmark and physical equations.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The framework introduces no new physical entities but relies on standard thin-shell approximations common in the field and an optional efficiency parameter.

free parameters (1)
  • shock-efficiency
    Optional time-dependent prescription for luminosity calculation mentioned in the abstract.
axioms (2)
  • domain assumption Thin-shell equations of motion govern the ejecta-CSM collision dynamics
    Core of the framework for solving motion as stated in the abstract.
  • domain assumption CSM can be treated as static finite shells for transport calculations
    Used in the finite-shell transport mode for photon diffusion and shock emergence.

pith-pipeline@v0.9.0 · 5866 in / 1591 out tokens · 86968 ms · 2026-05-20T04:27:13.057297+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

99 extracted references · 99 canonical work pages · 46 internal anchors

  1. [1]

    , keywords =

    REDBACK: a Bayesian inference software package for electromagnetic transients. , keywords =. doi:10.1093/mnras/stae1238 , archivePrefix =. 2308.12806 , primaryClass =

    work page doi:10.1093/mnras/stae1238

  2. [2]

    D., 2007, @doi [Computing in Science & Engineering] 10.1109/MCSE.2007.55 , 9, 90

    Matplotlib: A 2D Graphics Environment. Computing in Science and Engineering , keywords =. doi:10.1109/MCSE.2007.55 , adsurl =

    work page doi:10.1109/mcse.2007.55 2007

  3. [3]

    Array Programming with NumPy

    Array programming with NumPy. , keywords =. doi:10.1038/s41586-020-2649-2 , archivePrefix =. 2006.10256 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41586-020-2649-2 2006

  4. [4]

    Massive Stellar Mergers as Precursors of Hydrogen-rich Pulsational Pair Instability Supernovae

    Massive Stellar Mergers as Precursors of Hydrogen-rich Pulsational Pair Instability Supernovae. , keywords =. doi:10.3847/2041-8213/ab1bdf , archivePrefix =. 1903.02135 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/ab1bdf 2041

  5. [5]

    A magnetar model for the hydrogen-rich super-luminous supernova iPTF14hls

    A magnetar model for the hydrogen-rich super-luminous supernova iPTF14hls. , keywords =. doi:10.1051/0004-6361/201732402 , archivePrefix =. 1801.05340 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201732402

  6. [6]

    Energetic eruptions leading to a peculiar hydrogen-rich explosion of a massive star

    Energetic eruptions leading to a peculiar hydrogen-rich explosion of a massive star. , keywords =. doi:10.1038/nature24030 , archivePrefix =. 1711.02671 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature24030

  7. [7]

    Late-time observations of the extraordinary Type II supernova iPTF14hls

    Late-time observations of the extraordinary Type II supernova iPTF14hls. , keywords =. doi:10.1051/0004-6361/201833689 , archivePrefix =. 1806.10001 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201833689

  8. [8]

    Models for the Unusual Supernova iPTF14hls

    Models for the Unusual Supernova iPTF14hls. , keywords =. doi:10.3847/1538-4357/aad044 , archivePrefix =. 1801.08666 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aad044

  9. [9]

    A fallback accretion model for the unusual type II-P supernova iPTF14hls

    A Fallback Accretion Model for the Unusual Type II-P Supernova iPTF14hls. , keywords =. doi:10.3847/1538-4357/aadba4 , archivePrefix =. 1802.03982 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aadba4

  10. [10]

    Evidence for Pre-Existing Dust in the Bright Type IIn SN 2010jl

    Evidence for Pre-existing Dust in the Bright Type IIn SN 2010jl. , keywords =. doi:10.1088/0004-6256/142/2/45 , archivePrefix =. 1106.0537 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-6256/142/2/45

  11. [11]

    X-ray and radio emission from Type IIn supernova SN 2010jl

    X-Ray and Radio Emission from Type IIn Supernova SN 2010jl. , keywords =. doi:10.1088/0004-637X/810/1/32 , archivePrefix =. 1507.06059 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/810/1/32

  12. [12]

    SN 2010jl: Optical to hard X-ray observations reveal an explosion embedded in a ten solar mass cocoon

    SN 2010jl: Optical to Hard X-Ray Observations Reveal an Explosion Embedded in a Ten Solar Mass Cocoon. , keywords =. doi:10.1088/0004-637X/781/1/42 , archivePrefix =. 1307.2247 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/781/1/42

  13. [13]

    Handbook of Supernovae , year = 2017, editor =

    Thermal and Non-thermal Emission from Circumstellar Interaction. Handbook of Supernovae , year = 2017, editor =. doi:10.1007/978-3-319-21846-5_34 , adsurl =

    work page doi:10.1007/978-3-319-21846-5_34 2017

  14. [14]

    , keywords =

    Emission from Circumstellar Interaction in Normal Type II Supernovae. , keywords =. doi:10.1086/173557 , adsurl =

    work page doi:10.1086/173557

  15. [15]

    Circumstellar interaction in supernovae in dense environments - an observational perspective

    Circumstellar Interaction in Supernovae in Dense Environments An Observational Perspective. , keywords =. doi:10.1007/s11214-017-0461-6 , archivePrefix =. 1712.07405 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/s11214-017-0461-6

  16. [16]

    , keywords =

    SN 2009ip after a decade: the luminous blue variable progenitor is now gone. , keywords =. doi:10.1093/mnras/stac1669 , archivePrefix =. 2205.02896 , primaryClass =

    work page doi:10.1093/mnras/stac1669

  17. [17]

    , keywords =

    Analytic Light Curves of Dense CSM Shock Breakout and Cooling. , keywords =. doi:10.3847/1538-4357/ac771a , archivePrefix =. 2107.04048 , primaryClass =

    work page doi:10.3847/1538-4357/ac771a

  18. [18]

    A Massive Progenitor of the Luminous Type IIn Supernova 2010jl

    A Massive Progenitor of the Luminous Type IIn Supernova 2010jl. , keywords =. doi:10.1088/0004-637X/732/2/63 , archivePrefix =. 1011.4150 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/732/2/63

  19. [19]

    Central Bureau Electronic Telegrams , year = 2010, month = nov, volume =

    Possible Supernova in UGC 5189A. Central Bureau Electronic Telegrams , year = 2010, month = nov, volume =

    work page 2010

  20. [20]

    SN 2010jl in UGC 5189: Yet another luminous type IIn supernova in a metal-poor galaxy

    SN 2010jl in UGC 5189: Yet Another Luminous Type IIn Supernova in a Metal-poor Galaxy. , keywords =. doi:10.1088/0004-637X/730/1/34 , archivePrefix =. 1012.3461 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/730/1/34

  21. [21]

    Type IIn Supernova SN 2010jl: Optical Observations for Over 500 Days After Explosion

    Type IIn Supernova SN 2010jl: Optical Observations for over 500 Days after Explosion. , keywords =. doi:10.1088/0004-6256/144/5/131 , archivePrefix =. 1208.6078 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-6256/144/5/131

  22. [22]

    High Density Circumstellar Interaction in the Luminous Type IIn SN 2010jl: The first 1100 days

    High-density Circumstellar Interaction in the Luminous Type IIn SN 2010jl: The First 1100 Days. , keywords =. doi:10.1088/0004-637X/797/2/118 , archivePrefix =. 1312.6617 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/797/2/118

  23. [23]

    Bilby: A user-friendly Bayesian inference library for gravitational-wave astronomy

    BILBY: A User-friendly Bayesian Inference Library for Gravitational-wave Astronomy. , keywords =. doi:10.3847/1538-4365/ab06fc , archivePrefix =. 1811.02042 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/ab06fc

  24. [24]

    PyMultiNest: Python interface for MultiNest

    work page

  25. [25]

    , keywords =

    MULTINEST: an efficient and robust Bayesian inference tool for cosmology and particle physics. , keywords =. doi:10.1111/j.1365-2966.2009.14548.x , archivePrefix =. 0809.3437 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.14548.x 2009

  26. [26]

    SN 2015bn: a detailed multi-wavelength view of a nearby superluminous supernova

    SN 2015BN: A Detailed Multi-wavelength View of a Nearby Superluminous Supernova. , keywords =. doi:10.3847/0004-637X/826/1/39 , archivePrefix =. 1603.04748 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/826/1/39

  27. [27]

    Superluminous supernova 2015bn in the nebular phase: evidence for the engine-powered explosion of a stripped massive star

    Superluminous Supernova SN 2015bn in the Nebular Phase: Evidence for the Engine-powered Explosion of a Stripped Massive Star. , keywords =. doi:10.3847/2041-8205/828/2/L18 , archivePrefix =. 1608.02995 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8205/828/2/l18 2041

  28. [28]

    , keywords =

    Simulating the formation of Carinae's surrounding nebula through unstable triple evolution and stellar merger-induced eruption. , keywords =. doi:10.1093/mnras/stab571 , archivePrefix =. 2011.12434 , primaryClass =

    work page doi:10.1093/mnras/stab571 2011

  29. [29]

    On the role of continuum-driven eruptions in the evolution of very massive stars and Population III stars

    On the Role of Continuum-driven Eruptions in the Evolution of Very Massive Stars and Population III Stars. , keywords =. doi:10.1086/506523 , archivePrefix =. astro-ph/0606174 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/506523

  30. [30]

    A Blast Wave from the 1843 Eruption of Eta Carinae

    A blast wave from the 1843 eruption of Carinae. , keywords =. doi:10.1038/nature07269 , archivePrefix =. 0809.1678 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature07269

  31. [31]

    Hydrodynamical simulations and similarity relations for eruptive mass loss from massive stars

    Hydrodynamical simulations and similarity relations for eruptive mass-loss from massive stars. , keywords =. doi:10.1093/mnras/stz461 , archivePrefix =. 1902.06220 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz461 1902

  32. [32]

    , keywords =

    Multiple Peaks and a Long Precursor in the Type IIn Supernova 2021qqp: An Energetic Explosion in a Complex Circumstellar Environment. , keywords =. doi:10.3847/1538-4357/ad2854 , archivePrefix =. 2305.11168 , primaryClass =

    work page doi:10.3847/1538-4357/ad2854

  33. [33]

    , keywords =

    Supernova Precursor Emission and the Origin of Pre-explosion Stellar Mass Loss. , keywords =. doi:10.3847/1538-4357/ac892c , archivePrefix =. 2206.08377 , primaryClass =

    work page doi:10.3847/1538-4357/ac892c

  34. [34]

    , keywords =

    Light-curve Model for Luminous Red Novae and Inferences about the Ejecta of Stellar Mergers. , keywords =. doi:10.3847/1538-4357/ac6269 , archivePrefix =. 2202.10478 , primaryClass =

    work page doi:10.3847/1538-4357/ac6269

  35. [35]

    The Expulsion of Stellar Envelopes in Core-Collapse Supernovae

    The Expulsion of Stellar Envelopes in Core-Collapse Supernovae. , keywords =. doi:10.1086/306571 , archivePrefix =. astro-ph/9807046 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/306571

  36. [36]

    , keywords =

    CHIPS: Complete History of Interaction-powered Supernovae. , keywords =. doi:10.3847/1538-4357/ac60fe , archivePrefix =. 2109.05871 , primaryClass =

    work page doi:10.3847/1538-4357/ac60fe

  37. [37]

    An Analytic Bolometric Light Curve Model of Interaction-Powered Supernovae and its Application to Type IIn Supernovae

    An analytic bolometric light curve model of interaction-powered supernovae and its application to Type IIn supernovae. , keywords =. doi:10.1093/mnras/stt1392 , archivePrefix =. 1307.2644 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt1392

  38. [38]

    , keywords =

    Self-similar solutions for the interaction of stellar ejecta with an external medium. , keywords =. doi:10.1086/160126 , adsurl =

    work page doi:10.1086/160126

  39. [39]

    , keywords =

    Type IIn Supernova Light Curves Powered by Forward and Reverse Shocks. , keywords =. doi:10.3847/1538-4357/ab40ba , archivePrefix =. 1907.05166 , primaryClass =

    work page doi:10.3847/1538-4357/ab40ba 1907

  40. [40]

    Interacting Supernovae and Supernova Impostors. SN 2009ip, is this the end?

    Interacting Supernovae and Supernova Impostors: SN 2009ip, is this the End?. , keywords =. doi:10.1088/0004-637X/767/1/1 , archivePrefix =. 1210.3568 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/767/1/1

  41. [41]

    Diversity of Luminous Supernovae from Non-Steady Mass Loss

    Diversity of Luminous Supernovae from Non-steady Mass Loss. , keywords =. doi:10.1088/0004-637X/747/2/118 , archivePrefix =. 1110.3807 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/747/2/118

  42. [42]

    , keywords =

    Finding the Fuse: Prospects for the Detection and Characterization of Hydrogen-rich Core-collapse Supernova Precursor Emission with the LSST. , keywords =. doi:10.3847/1538-4357/ad9748 , archivePrefix =. 2408.13314 , primaryClass =

    work page doi:10.3847/1538-4357/ad9748

  43. [43]

    Encyclopedia of Astrophysics , year = 2026, volume =

    Core-collapse supernovae. Encyclopedia of Astrophysics , year = 2026, volume =. doi:10.1016/B978-0-443-21439-4.00090-0 , adsurl =

    work page doi:10.1016/b978-0-443-21439-4.00090-0 2026

  44. [44]

    Handbook of Supernovae , year = 2017, editor =

    Neutrino-Driven Explosions. Handbook of Supernovae , year = 2017, editor =. doi:10.1007/978-3-319-21846-5_109 , adsurl =

    work page doi:10.1007/978-3-319-21846-5_109 2017

  45. [45]

    Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars

    Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars. , keywords =. doi:10.1146/annurev-astro-081913-040025 , archivePrefix =. 1402.1237 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev-astro-081913-040025

  46. [46]

    Late-time spectral line formation in Type IIb supernovae, with application to SN 1993J, SN 2008ax, and SN 2011dh

    Late-time spectral line formation in Type IIb supernovae, with application to SN 1993J, SN 2008ax, and SN 2011dh. , keywords =. doi:10.1051/0004-6361/201423983 , archivePrefix =. 1408.0732 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201423983

  47. [47]

    , keywords =

    Multiwavelength View of the Type IIn Zoo: Optical to X-Ray Emission Model of Interaction-powered Supernovae. , keywords =. doi:10.3847/1538-4357/abfaf8 , archivePrefix =. 2103.08338 , primaryClass =

    work page doi:10.3847/1538-4357/abfaf8

  48. [48]

    , keywords =

    The La Silla Schmidt Southern Survey. , keywords =. doi:10.1088/1538-3873/ae02c5 , archivePrefix =. 2503.14579 , primaryClass =

    work page doi:10.1088/1538-3873/ae02c5

  49. [49]

    Fast & slow winds from supergiants and Luminous Blue Variables

    Fast and slow winds from supergiants and luminous blue variables. , keywords =. doi:10.1051/0004-6361/201833352 , archivePrefix =. 1808.06612 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201833352

  50. [50]

    The Zwicky Transient Facility: System Overview, Performance, and First Results

    The Zwicky Transient Facility: System Overview, Performance, and First Results. , keywords =. doi:10.1088/1538-3873/aaecbe , archivePrefix =. 1902.01932 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1538-3873/aaecbe 1902

  51. [51]

    , keywords =

    SN 2023xgo: Helium-rich Type Icn or Carbon-Flash Type Ibn supernova?. , keywords =. doi:10.1093/mnras/staf1517 , archivePrefix =. 2506.10700 , primaryClass =

    work page doi:10.1093/mnras/staf1517

  52. [52]

    SN 2020aeuh as a SN Ia-CSM-C/O?

    A thermonuclear supernova interacting with hydrogen- and helium-deficient circumstellar material. SN 2020aeuh as a SN Ia-CSM-C/O?. arXiv e-prints , keywords =. doi:10.48550/arXiv.2507.08532 , archivePrefix =. 2507.08532 , primaryClass =

    work page doi:10.48550/arxiv.2507.08532

  53. [53]

    , keywords =

    A Systematic Study of Ia-CSM Supernovae from the ZTF Bright Transient Survey. , keywords =. doi:10.3847/1538-4357/acbc16 , archivePrefix =. 2301.04637 , primaryClass =

    work page doi:10.3847/1538-4357/acbc16

  54. [54]

    Type Ia Supernovae Strongly Interacting with Their Circumstellar Medium

    Type Ia Supernovae Strongly Interacting with Their Circumstellar Medium. , keywords =. doi:10.1088/0067-0049/207/1/3 , archivePrefix =. 1304.0763 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/207/1/3

  55. [55]

    Transient Name Server Classification Report , keywords =

    REFITT Transient Classification Report for 2021-03-18. Transient Name Server Classification Report , keywords =

    work page 2021

  56. [56]

    Nature Reviews Methods Primers , keywords =

    Nested sampling for physical scientists. Nature Reviews Methods Primers , keywords =. doi:10.1038/s43586-022-00121-x , archivePrefix =. 2205.15570 , primaryClass =

    work page doi:10.1038/s43586-022-00121-x

  57. [57]

    , keywords =

    Constraining Type Ia supernova explosions and early flux excesses with the Zwicky Transient Factory. , keywords =. doi:10.1093/mnras/stac558 , archivePrefix =. 2202.12914 , primaryClass =

    work page doi:10.1093/mnras/stac558

  58. [58]

    , keywords =

    Very late-time spectroscopy of SN 2009ip: Constraints on the ongoing H emission. , keywords =. doi:10.1051/0004-6361/202347319 , archivePrefix =. 2308.07370 , primaryClass =

    work page doi:10.1051/0004-6361/202347319

  59. [59]

    Discovery of Precursor LBV Outbursts in Two Recent Optical Transients: The Fitfully Variable Missing Links UGC 2773-OT and SN 2009ip

    Discovery of Precursor Luminous Blue Variable Outbursts in Two Recent Optical Transients: The Fitfully Variable Missing Links UGC 2773-OT and SN 2009ip. , keywords =. doi:10.1088/0004-6256/139/4/1451 , archivePrefix =. 0909.4792 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-6256/139/4/1451

  60. [60]

    The Diversity of Massive Star Outbursts. I. Observations of SN2009ip, UGC 2773 OT2009-1, and Their Progenitors. , keywords =. doi:10.1088/0004-637X/732/1/32 , archivePrefix =. 1002.0635 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/732/1/32

  61. [61]

    SN 2009ip \'a la PESSTO: No evidence for core-collapse yet

    SN 2009ip \`a la PESSTO: no evidence for core collapse yet. , keywords =. doi:10.1093/mnras/stt813 , archivePrefix =. 1303.3453 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt813

  62. [62]

    The Unprecedented 2012 Outburst of SN 2009ip: A Luminous Blue Variable Becomes a True Supernova

    The unprecedented 2012 outburst of SN 2009ip: a luminous blue variable star becomes a true supernova. , keywords =. doi:10.1093/mnras/stt009 , archivePrefix =. 1209.6320 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt009 2012

  63. [63]

    SN2009ip: Constraints on the progenitor mass-loss rate

    SN 2009ip: Constraints on the Progenitor Mass-loss Rate. , keywords =. doi:10.1088/0004-637X/768/1/47 , archivePrefix =. 1303.3894 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/768/1/47

  64. [64]

    Precursors prior to Type IIn supernova explosions are common: precursor rates, properties, and correlations

    Precursors Prior to Type IIn Supernova Explosions are Common: Precursor Rates, Properties, and Correlations. , keywords =. doi:10.1088/0004-637X/789/2/104 , archivePrefix =. 1401.5468 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/789/2/104

  65. [65]

    , keywords =

    Synchrotron Self-Absorption in Radio Supernovae. , keywords =. doi:10.1086/305676 , adsurl =

    work page doi:10.1086/305676

  66. [66]

    Radiative processes in astrophysics

    work page

  67. [67]

    Theoretical Models of Optical Transients. I. A Broad Exploration of the Duration-Luminosity Phase Space. , keywords =. doi:10.3847/1538-4357/aa8fcb , archivePrefix =. 1707.08132 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aa8fcb

  68. [68]

    Research Notes of the American Astronomical Society , keywords =

    Extended Self-similar Solution for Circumstellar Material-supernova Ejecta Interaction. Research Notes of the American Astronomical Society , keywords =. doi:10.3847/2515-5172/ab7128 , archivePrefix =. 2008.10397 , primaryClass =

    work page doi:10.3847/2515-5172/ab7128 2008

  69. [69]

    Analytical Light Curve Models of Super-Luminous Supernovae: chi^2-Minimizations of Parameter Fits

    Analytical Light Curve Models of Superluminous Supernovae: ^ 2 -minimization of Parameter Fits. , keywords =. doi:10.1088/0004-637X/773/1/76 , archivePrefix =. 1306.3447 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/773/1/76

  70. [70]

    arXiv e-prints , keywords =

    SN Ia-CSM 2020aeuh: Massive binary C/O WD merger?. arXiv e-prints , keywords =. doi:10.48550/arXiv.2510.16840 , archivePrefix =. 2510.16840 , primaryClass =

    work page doi:10.48550/arxiv.2510.16840

  71. [71]

    , keywords =

    iPTF14hls as a variable hyper-wind from a very massive star. , keywords =. doi:10.1093/mnras/stz3122 , archivePrefix =. 1911.01740 , primaryClass =

    work page doi:10.1093/mnras/stz3122 1911

  72. [72]

    , keywords =

    Presupernova Evolution in Massive Interacting Binaries. , keywords =. doi:10.1086/171341 , adsurl =

    work page doi:10.1086/171341

  73. [73]

    , keywords =

    Interacting supernovae from wide massive binary systems. , keywords =. doi:10.1051/0004-6361/202347646 , archivePrefix =. 2308.01819 , primaryClass =

    work page doi:10.1051/0004-6361/202347646

  74. [74]

    , keywords =

    Nested sampling with normalizing flows for gravitational-wave inference. , keywords =. doi:10.1103/PhysRevD.103.103006 , archivePrefix =. 2102.11056 , primaryClass =

    work page doi:10.1103/physrevd.103.103006

  75. [75]

    The Visual Light Curve, 1595-2000

    The Historical Record of Carinae I. The Visual Light Curve, 1595-2000. Journal of Astronomical Data , keywords =

    work page 2000

  76. [76]

    arXiv e-prints , keywords =

    TransFit-CSM: A Fast, Physically Consistent Framework for Interaction-Powered Transients. arXiv e-prints , keywords =. doi:10.48550/arXiv.2511.13265 , archivePrefix =. 2511.13265 , primaryClass =

    work page doi:10.48550/arxiv.2511.13265

  77. [77]

    , keywords =

    Radiative Acceleration of Dense Circumstellar Material in Interacting Supernovae. , keywords =. doi:10.3847/1538-4357/acdb71 , archivePrefix =. 2301.10667 , primaryClass =

    work page doi:10.3847/1538-4357/acdb71

  78. [78]

    , keywords =

    Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C. , keywords =. doi:10.3847/1538-4357/ad8ac8 , archivePrefix =. 2410.17699 , primaryClass =

    work page doi:10.3847/1538-4357/ad8ac8

  79. [79]

    , keywords =

    Seven Years of Coordinated Chandra-NuSTAR Observations of SN 2014C Unfold the Extreme Mass-loss History of Its Stellar Progenitor. , keywords =. doi:10.3847/1538-4357/ac8b14 , archivePrefix =. 2206.00842 , primaryClass =

    work page doi:10.3847/1538-4357/ac8b14

  80. [80]

    , keywords =

    Supernova explosions interacting with aspherical circumstellar material: implications for light curves, spectral line profiles, and polarization. , keywords =. doi:10.1051/0004-6361/202039073 , archivePrefix =. 2008.13169 , primaryClass =

    work page doi:10.1051/0004-6361/202039073 2008

Showing first 80 references.