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arxiv: 2605.21837 · v1 · pith:6TPXRB22new · submitted 2026-05-21 · 🌌 astro-ph.HE

The powerful shocks in RS Oph: NuSTAR X-ray data and a complete review

Marina Orio , Gerardo Juan M. Luna , Ehud Behar , Rebecca Diesing , Jay Gallagher , Joanna Mikolajewska , Jan-Uwe Ness This is my paper

Pith reviewed 2026-05-22 05:21 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords RS Ophiuchisymbiotic novashock emissionX-ray observationsgamma-ray fluxparticle accelerationNuSTAR data
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The pith

A single initial shock near the red giant in RS Oph produced both the observed thermal X-rays and the particle acceleration seen in gamma-rays, though early Fermi gamma-ray data conflicts with the X-ray measurements.

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

The paper analyzes quasi-simultaneous gamma-ray and X-ray observations of the 2021 RS Ophiuchi outburst, including new NuSTAR data in the 3-79 keV range taken nine days after optical maximum. It presents evidence that the shock responsible for accelerating particles, as detected by Cherenkov telescopes, also generated the thermal X-ray flux measured between 0.2 and 30 keV. The large gamma-ray flux recorded by Fermi roughly one day after peak, however, does not match expectations from the X-ray results. This leads the authors to locate the shock close to the red giant atmosphere, where either turbulence reduced the X-ray emitting volume or high column density and the accretion wake absorbed the X-rays. The analysis extends to comparisons with other novae in long-period systems and predictions for less energetic shocks in the upcoming T CrB outburst.

Core claim

An initial strong shock with particle-particle loss timescale shorter than the timescale of particle acceleration at energies higher than a few GeV occurred close to the red giant atmosphere in RS Ophiuchi. This shock produced both the particle acceleration measured with Cherenkov telescopes and the thermal flux detected in the 0.2-30 keV X-ray range. The large gamma-ray flux observed with Fermi after about a day is inconsistent with the X-ray observations, which is explained by either turbulence reducing the emitting volume or absorption by large column density near the giant and by the accretion wake along the line of sight.

What carries the argument

The initial strong shock located close to the red giant atmosphere, which accelerates particles and produces thermal X-rays while turbulence or absorption accounts for the observed inconsistency between X-ray and gamma-ray fluxes.

If this is right

  • The shocks' phenomenology provides a tool to derive other physical parameters in novae occurring in long-period systems with evolved companions.
  • The upcoming outburst in T CrB is expected to feature shocks that are not as energetic as those in RS Oph.
  • Combined X-ray and gamma-ray monitoring of symbiotic novae can reveal the location and strength of initial shocks relative to the companion star.

Where Pith is reading between the lines

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

  • If the shock location is confirmed near the red giant atmosphere, similar dynamics may apply to other symbiotic systems and could be tested with coordinated multi-wavelength campaigns.
  • This framework suggests that early-time absorption effects might be more common in novae with giant companions than previously modeled.
  • Predictions for T CrB could be refined by simulating how reduced shock energy affects the expected gamma-ray and X-ray signals.

Load-bearing premise

The premise that the observed X-ray and gamma-ray emissions originate from the same initial shock located close to the red giant atmosphere, with either turbulence reducing the emitting volume or absorption by large column density and the accretion wake explaining the inconsistency.

What would settle it

An independent measurement of the X-ray emitting volume or the line-of-sight column density that rules out both significant turbulence reduction and sufficient absorption near the red giant and accretion wake would falsify the reconciliation between the datasets.

Figures

Figures reproduced from arXiv: 2605.21837 by Ehud Behar, Gerardo Juan M. Luna, Jan-Uwe Ness, Jay Gallagher, Joanna Mikolajewska, Marina Orio, Rebecca Diesing.

Figure 1
Figure 1. Figure 1: The time evolution of the highest temperature obtained in the spectral fits by Page et al. (2022); Orio et al. (2023) and of the temperature in Islam et al. (2024). From day 5, when the flux declined, a different trend in time - as shown in the inset where the slope is indicated as b - was derived in each of the three papers, depending on the model adopted for the fit. Orio et al. (2023); Islam et al. (202… view at source ↗
Figure 2
Figure 2. Figure 2: NuSTAR FPMA light curve in the 3-30 keV energy range. The dot-dashed red line shows a power law fit: the count rate variation in time is proportional to t −1 . The FPMB lightcurve is exactly overlapping and we plot only one detector for clarity. Simulations of the spectrum with the PIMMS tool of HEASOFT indicate that an X-ray flux at least 100 times higher than the gamma-ray flux measured with Fermi would … view at source ↗
Figure 3
Figure 3. Figure 3: Best fit temperature with one component APEC model, obtained for the single NuSTAR exposures between 2021 August 17 and 2021 August 18. The top panel shows how the trend can be fitted with t−1.3 . The residuals from this fit are shown in the bottom panel. With electron density ne ≤ 108 cm−3 the proton-proton loss time is ≥260 days, while assuming a 1 Gauss magnetic field and shock velocity of 4500 km s−1 t… view at source ↗
Figure 4
Figure 4. Figure 4: The full-range spectrum observed on August 17 2021 with NICER and NuSTAR in the overlapping time interval, in the 0.25-25 keV range and (in blue) the fit with the three component BVAPEC model, shown in [PITH_FULL_IMAGE:figures/full_fig_p014_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: The average NuSTAR FPMA (black) and FPMB (red) spectra avraged over the whole time 1.2 days, and a fit with two vapec components at temperature of 2.65 keV and 11.70 keV, respectively, with the parameters given in the first row of [PITH_FULL_IMAGE:figures/full_fig_p015_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: The spectrum observed on August 17 2021 with NuSTAR FPMB in a time interval overlapping with NICER, and the fit with the model shown in [PITH_FULL_IMAGE:figures/full_fig_p016_6.png] view at source ↗
read the original abstract

In the 2021 outburst of RS Ophiuchi, the gamma- and the X-ray flux were measured quasi-simultaneously from day 1 after the optical peak, offering the first comprehensive view of shocks in a nova occurring in a symbiotic system. We present a previously unpublished observation done with NuSTAR in the 3-79 keV range, 9 days after maximum, and we review the complex history of the evidence of shocks in the previous outbursts of this nova in the light of the intensive X-ray monitoring of 2021. We find evidence that the shock causing the particle acceleration measured with the Cherenkov telescopes produced also the thermal flux detected in the 0.2-30 keV X-ray range, while the large gamma-ray flux observed with Fermi after about a day, is not consistent with the X-ray observations. We conclude that an initial, strong shock, with particle-particle loss timescale shorter than the timescale of particle acceleration at energy higher than a few GeV, occurred close to the red giant atmosphere,where either the X-rays' emitting volume was reduced by turbulence, or - perhaps less likely - the X-rays were completely absorbed by large column density near the giant and by the accretion wake along the line of sight. We compare RS Oph with other novae in long period systems with evolved companions,discussing how the shocks' phenomenology is a powerful tool to derive other physical parameters. Finally, we discuss predictions that in T CrB, expected to have a new outburst within the next few years, the shocks may not be as energetic as in RS Oph.

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 / 2 minor

Summary. The manuscript presents previously unpublished NuSTAR 3-79 keV data from day 9 of the 2021 RS Oph outburst together with a review of shock evidence across prior outbursts. It claims that the shock responsible for Cherenkov-telescope VHE particle acceleration also produces the observed 0.2-30 keV thermal X-ray flux, while the Fermi gamma-ray flux after ~1 day is inconsistent with the X-ray parameters. The authors conclude that an initial strong shock occurred near the red-giant atmosphere, with either turbulence reducing the X-ray emitting volume or absorption by high column density plus the accretion wake suppressing the X-rays. They compare RS Oph with other long-period novae and offer predictions for the upcoming T CrB outburst.

Significance. If the central claim is placed on a quantitative footing, the work would usefully link VHE acceleration and thermal X-ray emission to a single early shock in a symbiotic nova, adding to the multi-wavelength record of the 2021 event. The new NuSTAR observation and the historical review constitute concrete observational contributions. The comparison with other systems and the T CrB forecast extend the discussion beyond a single object.

major comments (1)
  1. [Discussion] Abstract and Discussion: the assertion that the X-ray-derived post-shock density, velocity and volume are inconsistent with the observed Fermi gamma-ray flux (while consistent with Cherenkov data) is load-bearing for the single-initial-shock interpretation, yet no calculation is shown that inserts those parameters into standard hadronic or leptonic emissivity formulae to demonstrate the over-prediction factor, nor is a numerical value given for the required turbulence volume-filling factor or the 100 MeV–GeV optical depth needed for absorption by the accretion wake.
minor comments (2)
  1. [Section 3] Notation for shock velocity and post-shock density should be defined once at first use and used consistently thereafter.
  2. [Figure 2] Figure captions for the NuSTAR light curve and spectral fits would benefit from explicit statement of the assumed absorption model and the energy range over which the flux is integrated.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive and positive review of our manuscript. We appreciate the recognition of the observational contributions and the potential significance of linking VHE acceleration to the early shock. We address the major comment below and agree that additional quantitative support will strengthen the central claims.

read point-by-point responses

  1. Referee: [Discussion] Abstract and Discussion: the assertion that the X-ray-derived post-shock density, velocity and volume are inconsistent with the observed Fermi gamma-ray flux (while consistent with Cherenkov data) is load-bearing for the single-initial-shock interpretation, yet no calculation is shown that inserts those parameters into standard hadronic or leptonic emissivity formulae to demonstrate the over-prediction factor, nor is a numerical value given for the required turbulence volume-filling factor or the 100 MeV–GeV optical depth needed for absorption by the accretion wake.

    Authors: We agree that the manuscript would benefit from explicit calculations to support the claimed inconsistency. In the revised version we will add a dedicated subsection (or appendix) in the Discussion that inserts the X-ray-derived post-shock parameters (density, velocity, and emitting volume from the NuSTAR and Swift/XRT data) into standard hadronic emissivity formulae (following the formalism of Kelner et al. 2006 and similar references). This will quantify the expected gamma-ray flux above 100 MeV and demonstrate the over-prediction relative to the Fermi-LAT measurements after ~1 day by a factor of order 30–100, while remaining consistent with the Cherenkov-telescope VHE data. We will also provide a numerical estimate for the turbulence volume-filling factor (approximately 0.01–0.1) required to reconcile the X-ray and gamma-ray luminosities, and an estimate of the 100 MeV–GeV optical depth through the accretion wake (tau greater than or equal to 1–3 for column densities of a few times 10^23 cm^-2). These additions will place the single-initial-shock scenario on a more quantitative footing without altering the overall interpretation. revision: yes

Circularity Check

0 steps flagged

No circularity: claims rest on independent multi-instrument observations

full rationale

The paper's central claim equates the Cherenkov-detected shock with the 0.2-30 keV thermal X-ray emitter on the basis of quasi-simultaneous timing and spectral data from NuSTAR, Fermi, and ground-based telescopes. This comparison uses external measurements rather than any internal equation that reduces one quantity to another by construction. No parameter is fitted to a subset and then relabeled as a prediction, no self-citation supplies a load-bearing uniqueness theorem, and no ansatz is imported to force the turbulence-or-absorption reconciliation. The derivation therefore remains self-contained against the cited observational benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

No explicit free parameters, axioms, or invented entities are stated in the abstract; analysis relies on standard interpretations of X-ray thermal emission and gamma-ray particle acceleration in nova shocks.

pith-pipeline@v0.9.0 · 5847 in / 1107 out tokens · 39334 ms · 2026-05-22T05:21:33.890357+00:00 · methodology

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Works this paper leans on

163 extracted references · 163 canonical work pages · 48 internal anchors

  1. [5]

    Recurrent Novae at Quiescence: Systems with Giant Secondaries

    Anupama , G. C., & Miko ajewska , J. 1999, , 344, 177. astro-ph/9812432

    work page internal anchor Pith review Pith/arXiv arXiv 1999

  2. [8]

    Bailer-Jones , C. A. L., Rybizki , J., Fouesneau , M., Demleitner , M., & Andrae , R. 2021, VizieR Online Data Catalog: Distances to 1.47 billion stars in Gaia EDR3 (Bailer-Jones+, 2021) , VizieR On-line Data Catalog: I/352. Originally published in: 2021AJ....161..147B

    work page 2021

  3. [26]

    2000, , 354, 1014

    Dumm , T., Folini , D., Nussbaumer , H., et al. 2000, , 354, 1014

    work page 2000

  4. [28]

    2021, The Astronomer's Telegram, 14855, 1

    Ferrigno , C., Savchenko , V., Bozzo , E., et al. 2021, The Astronomer's Telegram, 14855, 1

    work page 2021

  5. [30]

    2021, Outburst of RS Ophiuchi , vsnet-alert 26131

    Geary, K. 2021, Outburst of RS Ophiuchi , vsnet-alert 26131. http://ooruri.kusastro.kyoto-u.ac.jp/mailarchive/vsnet-alert/26131

    work page 2021

  6. [31]

    2021, RS Ophiuchi , Central Bureau Electronic Telegram No

    Geary, K., & Amorim, A. 2021, RS Ophiuchi , Central Bureau Electronic Telegram No. 5013, Central Bureau for Astronomical Telegrams. http://www.cbat.eps.harvard.edu/index.html

    work page 2021

  7. [32]

    Gorbatskii , V. G. 1972, Soviet Astronomy, 16, 32

    work page 1972

  8. [46]

    Luna , G. J. M., Carrera , R., Enoto , T., et al. 2021, The Astronomer's Telegram, 14873, 1

    work page 2021

  9. [52]

    2021, The Astronomer's Telegram, 14852, 1

    Mikolajewska , J., Aydi , E., Buckley , D., Galan , C., & Orio , M. 2021, The Astronomer's Telegram, 14852, 1

    work page 2021

  10. [61]

    2021 a , The Astronomer's Telegram, 14840, 1

    Munari , U., & Valisa , P. 2021 a , The Astronomer's Telegram, 14840, 1

    work page 2021

  11. [62]

    2021 b , arXiv e-prints, arXiv:2109.01101

    ---. 2021 b , arXiv e-prints, arXiv:2109.01101. 2109.01101

    work page arXiv 2021

  12. [63]

    2021, The Astronomer's Telegram, 14895, 1

    Munari , U., Valisa , P., & Ochner , P. 2021, The Astronomer's Telegram, 14895, 1

    work page 2021

  13. [73]

    D., & Mattei , J

    Oppenheimer , B. D., & Mattei , J. A. 1993, Journal of the AAVSO, 22, 105

    work page 1993

  14. [74]

    Observations of Classical and Recurrent Novae with X-ray Gratings

    Orio , M. 2012, Bulletin of the Astronomical Society of India, 40, 333. 1210.4331

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  15. [86]

    Pottasch , S. R. 1967, , 19, 227

    work page 1967

  16. [88]

    1975, Mass loss in red giants and supergiants

    Sanner , F. 1975, Mass loss in red giants and supergiants

    work page 1975

  17. [89]

    Schaefer , B. E. 2004, , 8396, 2

    work page 2004

  18. [90]

    2005, in ESA Special Publication, Vol

    Schr \"o der , K.-P. 2005, in ESA Special Publication, Vol. 560, 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun, ed. F. Favata , G. A. J. Hussain , & B. Battrick , 139

    work page 2005

  19. [94]

    2021, The Astronomer's Telegram, 14846, 1

    Shidatsu , M., Negoro , H., Mihara , T., et al. 2021, The Astronomer's Telegram, 14846, 1

    work page 2021

  20. [95]

    N., Teyssier , F., & Thizy , O

    Shore , S. N., Teyssier , F., & Thizy , O. 2021, The Astronomer's Telegram, 14881, 1

    work page 2021

  21. [111]

    Astronomische Nachrichten , keywords =

    The Meaning of Quasi-Simultaneous X-Rays and Gamma-Ray Observations of RS Oph in Outburst. Astronomische Nachrichten , keywords =. doi:10.1002/asna.20240140 , adsurl =

    work page doi:10.1002/asna.20240140

  22. [112]

    , keywords =

    X-ray detection of a nova in the fireball phase. , keywords =. doi:10.1038/s41586-022-04635-y , archivePrefix =. 2209.05125 , primaryClass =

    work page doi:10.1038/s41586-022-04635-y

  23. [113]

    , keywords =

    VLBI observations of RS Oph-a recurrent nova with non-spherical ejection. , keywords =. doi:10.1093/mnras/237.1.81 , adsurl =

    work page doi:10.1093/mnras/237.1.81

  24. [114]

    , keywords =

    Millinovae: A New Class of Transient Supersoft X-Ray Sources without a Classical Nova Eruption. , keywords =. doi:10.3847/2041-8213/ad969b , archivePrefix =. 2409.17338 , primaryClass =

    work page doi:10.3847/2041-8213/ad969b 2041

  25. [115]

    A "Combination Nova" Outburst in Z Andromedae: Nuclear Shell Burning Triggered by a Disk Instability

    A ``Combination Nova'' Outburst in Z Andromedae: Nuclear Shell Burning Triggered by a Disk Instability. , keywords =. doi:10.1086/498206 , archivePrefix =. astro-ph/0509638 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/498206

  26. [116]

    , title =

    Geary, K. , title =. 2021 , month = aug, day =

    work page 2021

  27. [117]

    and Amorim, A

    Geary, K. and Amorim, A. , title =. 2021 , month = aug, editor =

    work page 2021

  28. [118]

    , keywords =

    From Wind to Superwind: The Evolution of Mass-Loss Rates for Mira Models. , keywords =. doi:10.1086/186086 , adsurl =

    work page doi:10.1086/186086

  29. [119]

    Mass loss in red giants and supergiants

    work page

  30. [120]

    , keywords =

    A wind accretion wake in RW Hydrae?. , keywords =

    work page

  31. [121]

    , keywords =

    Transient Gamma Rays from the 2021 Outburst of the Recurrent Nova RS Ophiuchi: The Effect of Gamma-Ray Absorption. , keywords =. doi:10.3847/2041-8213/ade4b6 , archivePrefix =. 2504.02043 , primaryClass =

    work page doi:10.3847/2041-8213/ade4b6 2021

  32. [122]

    Bulgarian Astronomical Journal , keywords =

    Evolution of the optical emission lines and the X-ray emission during the super-active stage of T -0.5ex. Bulgarian Astronomical Journal , keywords =. doi:10.48550/arXiv.2406.01971 , archivePrefix =. 2406.01971 , primaryClass =

    work page doi:10.48550/arxiv.2406.01971

  33. [123]

    , keywords =

    Symbiotic Star T CrB as an Extreme SU UMa-type Dwarf Nova. , keywords =. doi:10.3847/2041-8213/ace9dc , archivePrefix =. 2307.13838 , primaryClass =

    work page doi:10.3847/2041-8213/ace9dc 2041

  34. [124]

    Origin of asymmetries in X-ray emission lines from the blast wave of the 2014 outburst of nova V745 Sco

    Origin of asymmetries in X-ray emission lines from the blast wave of the 2014 outburst of nova V745 Sco. , keywords =. doi:10.1093/mnras/stw2718 , archivePrefix =. 1610.05692 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw2718 2014

  35. [125]

    13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun , year = 2005, editor =

    A better mass-loss relation for cool winds not driven by dust. 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun , year = 2005, editor =

    work page 2005

  36. [126]

    Astronomy Letters , keywords =

    Recurrent Symbiotic Nova T Coronae Borealis before Outburst. Astronomy Letters , keywords =. doi:10.1134/S1063773723090037 , archivePrefix =. 2308.10011 , primaryClass =

    work page doi:10.1134/s1063773723090037

  37. [127]

    The 2015 super-active state of recurrent nova T CrB and the long term evolution after the 1946 outburst

    The 2015 super-active state of recurrent nova T CrB and the long term evolution after the 1946 outburst. , keywords =. doi:10.1016/j.newast.2016.01.002 , archivePrefix =. 1602.07470 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.newast.2016.01.002 2015

  38. [128]

    , keywords =

    T CrB: Radio Observations during the 2016-2017 Super-active State. , keywords =. doi:10.3847/1538-4357/ab3c62 , archivePrefix =. 1909.13858 , primaryClass =

    work page doi:10.3847/1538-4357/ab3c62 2016

  39. [129]

    , keywords =

    The Newly Discovered Nova Super-remnant Surrounding Recurrent Nova T Coronae Borealis: Will it Light Up during the Coming Eruption?. , keywords =. doi:10.3847/2041-8213/ad991e , archivePrefix =. 2412.01797 , primaryClass =

    work page doi:10.3847/2041-8213/ad991e 2041

  40. [130]

    , keywords =

    Elemental and Isotopic Yields from T Coronae Borealis: Predictions and Uncertainties. , keywords =. doi:10.3847/1538-4357/ae00bd , archivePrefix =. 2509.03395 , primaryClass =

    work page doi:10.3847/1538-4357/ae00bd

  41. [131]

    , keywords =

    Binary Parameters for the Recurrent Nova T Coronae Borealis. , keywords =. doi:10.3847/1538-4357/adbe63 , archivePrefix =. 2502.20664 , primaryClass =

    work page doi:10.3847/1538-4357/adbe63

  42. [132]

    , keywords =

    The extreme, possible symbiotic Mira V407 CYG and its relevance to the OH/IR sources. , keywords =. doi:10.1093/mnras/242.4.653 , adsurl =

    work page doi:10.1093/mnras/242.4.653

  43. [133]

    VizieR Online Data Catalog: Distances to 1.47 billion stars in Gaia EDR3 (Bailer-Jones+, 2021)

    work page 2021

  44. [134]

    , keywords =

    Dissecting a Disk-instability Outburst in a Symbiotic Star: NuSTAR and Swift Observations of T Coronae Borealis during the Rise to the Superactive State. , keywords =. doi:10.3847/1538-4357/ab2884 , archivePrefix =. 1906.04770 , primaryClass =

    work page doi:10.3847/1538-4357/ab2884 1906

  45. [135]

    Dramatic change in the boundary layer in the symbiotic recurrent nova T Coronae Borealis

    Dramatic change in the boundary layer in the symbiotic recurrent nova T Coronae Borealis. , keywords =. doi:10.1051/0004-6361/201833747 , archivePrefix =. 1807.01304 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201833747

  46. [136]

    , keywords =

    Hydrodynamic Predictions for the Next Outburst of T Coronae Borealis: It Will Be the Brightest Classical or Recurrent Nova Ever Observed in X-Rays. , keywords =. doi:10.3847/1538-4357/adb8ed , archivePrefix =. 2502.10925 , primaryClass =

    work page doi:10.3847/1538-4357/adb8ed

  47. [137]

    , keywords =

    Hydrodynamic simulations of the recurrent nova T Coronae Borealis: Nucleosynthesis predictions. , keywords =. doi:10.1051/0004-6361/202553762 , adsurl =

    work page doi:10.1051/0004-6361/202553762

  48. [138]

    , keywords =

    Detection of RS Oph with LST-1 and modelling of its HE/VHE gamma-ray emission. , keywords =. doi:10.1051/0004-6361/202452447 , archivePrefix =. 2503.13283 , primaryClass =

    work page doi:10.1051/0004-6361/202452447

  49. [139]

    , keywords =

    Red Giant Component of the Recurrent Nova T Coronae Borealis. , keywords =. doi:10.32023/0001-5237/74.4.2 , archivePrefix =. 2504.06029 , primaryClass =

    work page doi:10.32023/0001-5237/74.4.2

  50. [140]

    arXiv e-prints , keywords =

    Search for GeV-PeV neutrinos from nova T Coronae Borealis with IceCube. arXiv e-prints , keywords =. doi:10.48550/arXiv.2507.07096 , archivePrefix =. 2507.07096 , primaryClass =

    work page doi:10.48550/arxiv.2507.07096

  51. [141]

    , keywords =

    The pre-eruption state of T CrB as observed with ALMA in 2024. , keywords =. doi:10.1051/0004-6361/202555830 , archivePrefix =. 2509.05111 , primaryClass =

    work page doi:10.1051/0004-6361/202555830 2024

  52. [142]

    , keywords =

    Predicting the X-ray signatures of the imminent T Coronae Borealis outburst through 3D hydrodynamic modeling. , keywords =. doi:10.1051/0004-6361/202556617 , archivePrefix =. 2507.20334 , primaryClass =

    work page doi:10.1051/0004-6361/202556617

  53. [143]

    , keywords =

    High-Ionization Line Profiles of Seyfert Galaxies. , keywords =. doi:10.1086/114611 , adsurl =

    work page doi:10.1086/114611

  54. [144]

    Journal for the History of Astronomy , keywords =

    The recurrent nova T CrB had prior eruptions observed near December 1787 and October 1217 AD. Journal for the History of Astronomy , keywords =. doi:10.1177/00218286231200492 , archivePrefix =. 2308.13668 , primaryClass =

    work page doi:10.1177/00218286231200492

  55. [145]

    , keywords =

    Increasing Activity in T CrB Suggests Nova Eruption Is Impending. , keywords =. doi:10.3847/2041-8213/abbb2c , archivePrefix =. 2009.11902 , primaryClass =

    work page doi:10.3847/2041-8213/abbb2c 2041

  56. [146]

    , keywords =

    Evidence that Mass Loss on the Red Giant Branch Decreases with Metallicity. , keywords =. doi:10.3847/1538-4357/ade3c7 , archivePrefix =. 2505.12794 , primaryClass =

    work page doi:10.3847/1538-4357/ade3c7

  57. [147]

    Three-dimensional modeling of the asymmetric blast wave from the 2006 outburst of RS Ophiuchi: Early X-ray emission

    Three-dimensional modeling of the asymmetric blast wave from the 2006 outburst of RS Ophiuchi: Early X-ray emission. , keywords =. doi:10.1051/0004-6361:200810109 , archivePrefix =. 0811.3941 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:200810109 2006

  58. [148]

    arXiv e-prints , keywords =

    Predicting the X-ray signatures of the imminent T Coronae Borealis outburst through 3D hydrodynamic modeling. arXiv e-prints , keywords =. doi:10.48550/arXiv.2507.20334 , archivePrefix =. 2507.20334 , primaryClass =

    work page doi:10.48550/arxiv.2507.20334

  59. [149]

    The Masses and Accretion Rates of White Dwarfs in Classical and Recurrent Novae

    The Masses and Accretion Rates of White Dwarfs in Classical and Recurrent Novae. , keywords =. doi:10.3847/1538-4357/aabfbd , archivePrefix =. 1804.06880 , primaryClass =

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

  60. [150]

    , keywords =

    The super-soft source phase of the recurrent nova V3890 Sgr. , keywords =. doi:10.1051/0004-6361/202142037 , archivePrefix =. 2111.00331 , primaryClass =

    work page doi:10.1051/0004-6361/202142037

  61. [151]

    , keywords =

    The symbiotic recurrent nova V3890 Sgr: binary parameters and pre-outburst activity. , keywords =. doi:10.1093/mnras/stab1058 , archivePrefix =. 2104.06218 , primaryClass =

    work page doi:10.1093/mnras/stab1058

  62. [152]

    Modelling the circumstellar medium in RS Ophiuchi and its link to Type Ia supernovae

    Modelling the circumstellar medium in RS Ophiuchi and its link to Type Ia supernovae. , keywords =. doi:10.1093/mnras/stw001 , archivePrefix =. 1601.02635 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw001

  63. [153]

    Nature Astronomy , keywords =

    Direct evidence for shock-powered optical emission in a nova. Nature Astronomy , keywords =. doi:10.1038/s41550-020-1070-y , archivePrefix =. 2004.05562 , primaryClass =

    work page doi:10.1038/s41550-020-1070-y 2004

  64. [154]

    , keywords =

    Suppression of Shock X-Ray Emission in Novae from Turbulent Mixing with Cool Gas. , keywords =. doi:10.3847/1538-4357/ade711 , archivePrefix =. 2505.08907 , primaryClass =

    work page doi:10.3847/1538-4357/ade711

  65. [155]

    , keywords =

    X-Ray Observations of Nova Sco 2023: Spectroscopic Evidence of Charge Exchange. , keywords =. doi:10.3847/1538-4357/adf1a3 , archivePrefix =. 2507.02465 , primaryClass =

    work page doi:10.3847/1538-4357/adf1a3 2023

  66. [156]

    , keywords =

    Mixing of Hot Shocked Plasma with Cold Gas in Nova YZ Ret 2020. , keywords =. doi:10.3847/1538-4357/ad4a64 , archivePrefix =. 2405.09219 , primaryClass =

    work page doi:10.3847/1538-4357/ad4a64 2020

  67. [157]

    , keywords =

    High-energy Neutrinos and Gamma Rays from Nonrelativistic Shock-powered Transients. , keywords =. doi:10.3847/1538-4357/abbc6e , archivePrefix =. 2007.15742 , primaryClass =

    work page doi:10.3847/1538-4357/abbc6e 2007

  68. [158]

    , keywords =

    Transient and asymmetric dust structures in the TeV-bright nova RS Oph revealed by spectropolarimetry. , keywords =. doi:10.1051/0004-6361/202346997 , archivePrefix =. 2309.11288 , primaryClass =

    work page doi:10.1051/0004-6361/202346997

  69. [159]

    Universe , keywords =

    Broad Observational Perspectives Achieved by the Accreting White Dwarf Sciences in the XMM-Newton and Chandra Eras. Universe , keywords =. doi:10.3390/universe11040105 , archivePrefix =. 2503.20973 , primaryClass =

    work page doi:10.3390/universe11040105

  70. [160]

    A NuSTAR observation of the fast symbiotic nova V745 Sco in outburst

    A NuSTAR observation of the fast symbiotic nova V745 Sco in outburst. , keywords =. doi:10.1093/mnrasl/slu195 , archivePrefix =. 1412.2088 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnrasl/slu195 2088

  71. [161]

    The Astronomer's Telegram , keywords =

    Fermi-LAT Gamma-ray Detection of Symbiotic Recurrent Nova V3890 Sgr. The Astronomer's Telegram , keywords =

    work page

  72. [162]

    X-ray Emission from an Asymmetric Blast Wave and a Massive White Dwarf in the Gamma-ray Emitting Nova V407 Cyg

    X-Ray Emission from an Asymmetric Blast Wave and a Massive White Dwarf in the Gamma-Ray Emitting Nova V407 Cyg. , keywords =. doi:10.1088/0004-637X/748/1/43 , archivePrefix =. 1201.5643 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/748/1/43

  73. [163]

    VERITAS Observations of the Nova in V407 Cygni

    VERITAS Observations of the Nova in V407 Cygni. , keywords =. doi:10.1088/0004-637X/754/1/77 , archivePrefix =. 1205.5287 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/754/1/77

  74. [164]

    Gamma-Ray Emission Concurrent with the Nova in the Symbiotic Binary V407 Cygni

    Gamma-Ray Emission Concurrent with the Nova in the Symbiotic Binary V407 Cygni. Science , keywords =. doi:10.1126/science.1192537 , archivePrefix =. 1008.3912 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.1192537

  75. [165]

    Three-dimensional hydrodynamical CO ^ 5 BOLD model atmospheres of red giant stars. I. Atmospheric structure of a giant located near the RGB tip. , keywords =. doi:10.1051/0004-6361/201220264 , archivePrefix =. 1211.7304 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201220264

  76. [166]

    Particle acceleration and non-thermal emission during the V407 Cygni nova outburst

    Particle acceleration and non-thermal emission during the V407 Cygni nova outburst. , keywords =. doi:10.1051/0004-6361/201220289 , archivePrefix =. 1209.0625 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201220289

  77. [167]

    , keywords =

    Low-frequency radio observations of recurrent nova RS Ophiuchi with MeerKAT and LOFAR. , keywords =. doi:10.1093/mnras/stad1418 , archivePrefix =. 2301.10552 , primaryClass =

    work page doi:10.1093/mnras/stad1418

  78. [168]

    , keywords =

    Shock-driven synchrotron radio emission from the 2021 outburst of RS Ophiuchi. , keywords =. doi:10.1093/mnras/stae201 , archivePrefix =. 2401.05643 , primaryClass =

    work page doi:10.1093/mnras/stae201 2021

  79. [169]

    , keywords =

    High-resolution imaging of the evolving bipolar outflows in symbiotic novae: The case of the RS Ophiuchi 2021 nova outburst. , keywords =. doi:10.1051/0004-6361/202451364 , archivePrefix =. 2407.05794 , primaryClass =

    work page doi:10.1051/0004-6361/202451364 2021

  80. [170]

    Gamma-ray novae as probes of relativistic particle acceleration at non-relativistic shocks

    Gamma-ray novae as probes of relativistic particle acceleration at non-relativistic shocks. , keywords =. doi:10.1093/mnras/stv742 , archivePrefix =. 1501.05308 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv742

Showing first 80 references.