pith. sign in

arxiv: 2606.13202 · v1 · pith:LPC2VKOPnew · submitted 2026-06-11 · 🌌 astro-ph.SR

The first hours and days of the 2021 explosion of the recurrent symbiotic nova RS Ophiuchii

Augustin Skopal , Martin Vra\v{s}\v{t}\'ak , Francois Teyssier , Mitsugu Fujii , Sergei Shugarov , Miroslav \v{S}lechta , Marek Wolf This is my paper

Pith reviewed 2026-06-27 05:53 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords recurrent symbiotic novaRS Ophiuchibipolar ejectawhite dwarf rotationinternal shocksspectral energy distributiongamma-ray emissionpseudophotosphere
0
0 comments X

The pith

Bipolar ejecta in RS Oph form from white dwarf rotation and power shocks that reprocess into the pseudophotosphere.

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

The paper models the spectral energy distribution of the 2021 RS Ophiuchi explosion from nine hours before optical maximum through day 42, using optical spectroscopy, simultaneous BVRcIc photometry, and ultraviolet data from prior outbursts. The models show the ejecta developing a bipolar geometry with a flared, density-enhanced equatorial disk and low-density regions along the poles. Luminosity from internal shocks within the equatorial outflow matches the output of the warm white dwarf pseudophotosphere while that component is visible, indicating that reprocessed shock radiation supplies a substantial fraction of the observed light. The authors trace the origin of this geometry to the rotation of the accreting white dwarf, which also creates conditions for gamma-ray production inside the ejecta.

Core claim

Our SED models revealed an early stage of development of the ejecta bipolar structure, consisting of a flared, density-enhanced equatorial disk and low-density regions in bipolar directions. The comparability of the internal shocks' luminosity in the equatorial outflow, inferred from our model parameters, with the luminosity of the warm WD pseudophotosphere during its presence in the spectrum (until ∼day 42) confirmed that a significant part of its radiation originates from reprocessed shock emission. We explain the formation and evolution of the bipolar ejecta structure during RS Oph explosions by the rotation of the accreting WD. Such an ejecta structure provides a natural framework for th

What carries the argument

The bipolar ejecta structure with a flared density-enhanced equatorial disk and low-density bipolar regions, whose formation is attributed to rotation of the accreting white dwarf.

If this is right

  • Rotation of the accreting white dwarf sets the bipolar geometry of the ejecta in RS Oph explosions.
  • Internal shocks in the equatorial outflow reprocess energy that supplies a significant fraction of the pseudophotosphere luminosity until day 42.
  • The resulting structure generates strong internal shocks capable of producing gamma-ray emission inside the ejecta.
  • The same ejecta geometry and shock reprocessing operated in the 2006 and 1985 outbursts of RS Oph.

Where Pith is reading between the lines

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

  • If white dwarf spin controls the ejecta opening angle, future high-resolution observations could constrain the rotation period directly from the bipolar structure.
  • Gamma-ray monitoring campaigns timed to the first weeks after outburst could test the predicted internal-shock luminosities.
  • The reprocessing channel may operate in other recurrent novae and could reduce the need to invoke separate energy sources to match observed light curves.

Load-bearing premise

The observed spectrum can be decomposed into a flared equatorial disk plus low-density bipolar regions such that the calculated internal-shock luminosity directly accounts for the pseudophotosphere output without other major contributions.

What would settle it

High-resolution imaging or spectroscopy that shows no equatorial density enhancement matching the modeled parameters, or gamma-ray observations that yield fluxes inconsistent with the inferred shock luminosities during the first 42 days.

Figures

Figures reproduced from arXiv: 2606.13202 by Augustin Skopal, Francois Teyssier, Marek Wolf, Martin Vra\v{s}\v{t}\'ak, Miroslav \v{S}lechta, Mitsugu Fujii, Sergei Shugarov.

Figure 1
Figure 1. Figure 1: Comparison of V and visual LCs of RS Oph around the maxima of its explosions in 2021, 2006, and 1985. The gray curve is a third-degree polynomial that fits the V magnitudes around the 2021 maximum. The vertical dotted and dashed lines indicate the time of the brightness onset and its maximum, respectively ( [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Sketch for the RS Oph ejecta inferred from SED models (side view, Sect. 4.1). Due to the WD rotation, the wind is compressed and slowed down towards the equa￾tor at the expense of the polar directions, where we indicate a fast ionized wind (Sect. 4.2). The radius of the optically thick/thin compressed wind interface (i.e., the warm WDP, brown line) starts to shrink after the maximum due to its expansion an… view at source ↗
Figure 3
Figure 3. Figure 3: Examples of the observed (in magenta) and modeled (black lines) SEDs of RS Oph at selected dates from the onset of its 2021 outburst. The meaning of lines and symbols is as shown in the keys (top left panels). The solid blue line represents the radiation of the warm WDP, while the dotted blue line (from day 5.416) represents the radiation of the hot WDP (see Sect. 3.2). The spectrum of the giant (in orange… view at source ↗
Figure 4
Figure 4. Figure 4: Examples of SED models in the UV/optical/near-IR domain. Given the similarity of the RS Oph eruptions, our observations were supplemented with (near-)simultaneous observations of the previous two eruptions (in gray). Denotation of lines and points is the same as in [PITH_FULL_IMAGE:figures/full_fig_p010_4.png] view at source ↗
Figure 6
Figure 6. Figure 6: Mass-loss rate by the ionized part of the ejecta, M˙ WD (panel (a)), and its corresponding mass, Mneb (b). See Sects. 3.3 and 3.4. However, its reality is not supported by the M˙ WD values determined from EM. 3.4. Mass released by the ionized ejecta The mass of the ionized part of the ejecta can be es￾timated by integrating its outflow rate from the first detection of the nebular continuum on day 0.13 to o… view at source ↗
Figure 5
Figure 5. Figure 5: The B, V , and IC LCs (panel (a)), and evolution in LWD (b), R eff WD (c), and TWD (d) parameters from the onset of the RS Oph explosion, t0. Parameter values are in [PITH_FULL_IMAGE:figures/full_fig_p011_5.png] view at source ↗
Figure 7
Figure 7. Figure 7: Evolution of the Hα line parameters. Left: The broad component: The flux (panel (a)), its maximum height, Fmax, above the continuum (b), FWHM (c), and terminal velocities of the wings (d). The description is in Sect. 3.5.1 and the data in [PITH_FULL_IMAGE:figures/full_fig_p013_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Example of the evolution of the broad and narrow components of the hydrogen line profiles measured on UVES spectra. Left panel shows the Hα broad component measured on days 1.567 and 37.532. This comparison shows a significant narrowing of the line emission core (see [PITH_FULL_IMAGE:figures/full_fig_p014_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: The ratio of fluxes from the warm WDP, F warm WD , and the nebula, FN, at selected wavelengths, 3,600 ˚A, 4,040 ˚A, 4,700 ˚A, and 7,300 ˚A, given by SED models. The rapid decrease of this ratio indicates a rapid opening of bipo￾lar ionized regions (see Sects. 4.3). The vertical line denotes a sudden change of this ratio between days 3.395 and 3.759, reflecting a change in the physical parameters of the war… view at source ↗
Figure 10
Figure 10. Figure 10: shows a good agreement between the values of L warm WD and Lsh for vsh = 1 800 km s−1 . However, it is likely that the actual values of Lsh are smaller than the values of L warm WD determined directly from the spectrum, because the efficiency of generating shocks is expected to be higher near the equator due to the largest velocity difference, vf − vsh, than at higher latitudes of the slow outflow under t… view at source ↗
Figure 11
Figure 11. Figure 11: Evolution of the continuum fluxes, Fcont., at/around selected emission lines (see keys) given by SED models. The vertical dotted line indicates the time of the optical maximum (see [PITH_FULL_IMAGE:figures/full_fig_p022_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: The evolution of the RS Oph optical spectrum measured by the UVES spectrograph from day 0.617 to day 42.566. A strong nebular continuum is indicated by the Balmer jump in emission. It dominates the spectrum from day 3.7, when the overall continuum flattens (see also [PITH_FULL_IMAGE:figures/full_fig_p024_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Evolution of the Hα (left) and Hβ (right) line profiles during the first hours and days of the RS Oph explosion. Vertical gray lines denote the terminal velocity of the broad absorption component, while the dotted lines denote emission bumps located around ±2,500 km s−1 [PITH_FULL_IMAGE:figures/full_fig_p025_13.png] view at source ↗
read the original abstract

The accretion of matter on a massive white dwarf (WD) can lead to repeated nuclear explosions on its surface over a timescale of years to decades. The seventh explosion of the recurrent symbiotic nova RS Ophiuchi (RS Oph) was recorded on August 8, 2021. In this paper, we examine its early evolution, from 9 hours before its optical maximum until day 42. We achieved our goal by modeling the spectral energy distribution (SED) using optical spectroscopy and simultaneous $BVR_{\rm C}I_{\rm C}$ photometry, supplemented by $JHKL$ photometry and ultraviolet spectroscopy from previous explosions in 2006 and 1985. Our SED models revealed an early stage of development of the ejecta bipolar structure, consisting of a flared, density-enhanced equatorial disk and low-density regions in bipolar directions. The comparability of the internal shocks' luminosity in the equatorial outflow, inferred from our model parameters, with the luminosity of the warm WD pseudophotosphere during its presence in the spectrum (until $\sim$day 42) confirmed that a significant part of its radiation originates from reprocessed shock emission. We explain the formation and evolution of the bipolar ejecta structure during RS Oph explosions by the rotation of the accreting WD. Such an ejecta structure provides a natural framework for the generation of strong internal shocks and thus $\gamma$-ray emission inside the ejecta.

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

2 major / 0 minor

Summary. The paper models the spectral energy distribution (SED) of the 2021 RS Ophiuchi explosion from 9 hours before optical maximum to day 42, using optical spectroscopy, BVRcIc photometry, and supplementary JHKL/UV data from the 2006 and 1985 events. The models indicate an early bipolar ejecta structure consisting of a flared, density-enhanced equatorial disk and low-density bipolar regions. The authors infer that the luminosity of internal shocks in the equatorial outflow is comparable to the warm WD pseudophotosphere luminosity (present until ~day 42), confirming that a significant fraction of the pseudophotosphere radiation is reprocessed shock emission. They attribute the bipolar structure to rotation of the accreting WD and note that this geometry naturally generates internal shocks capable of producing gamma-ray emission.

Significance. If the SED decomposition and luminosity comparison hold, the work provides a physically motivated framework for the early geometry and energy budget of recurrent symbiotic novae, linking ejecta morphology directly to WD rotation and internal shocks. This could inform models of gamma-ray production in such systems and the role of reprocessing in the observed pseudophotosphere.

major comments (2)
  1. [Abstract] Abstract: The abstract states modeling results and conclusions but supplies no information on the functional form of the SED components, fitting procedure, error treatment, or validation against the data, so the support for the central claims cannot be assessed from available text.
  2. [Abstract] Abstract: The central claim that comparability of inferred internal shock luminosity (from equatorial outflow model parameters) to warm WD pseudophotosphere luminosity confirms reprocessing origin depends on the SED model correctly decomposing the flared density-enhanced equatorial disk plus low-density bipolar regions, and on the shock luminosity being computed such that it can be directly compared without unaccounted geometric factors, reprocessing efficiency <1, or contributions from the WD itself or other components. The model also incorporates JHKL and UV data from the 2006/1985 events, which may not match 2021 conditions exactly.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thorough and constructive review. We address the two major comments below. We agree that the abstract can be strengthened to better outline the modeling methodology and will revise it accordingly while preserving its concise nature.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The abstract states modeling results and conclusions but supplies no information on the functional form of the SED components, fitting procedure, error treatment, or validation against the data, so the support for the central claims cannot be assessed from available text.

    Authors: The abstract is intentionally brief to highlight the primary results and conclusions. Full details on the SED components (flared equatorial disk with enhanced density, low-density bipolar regions, and separate blackbody for the WD pseudophotosphere), the fitting procedure (chi-squared minimization to combined spectroscopy and BVRcIc photometry), error treatment (incorporating observational uncertainties and parameter covariances), and validation (via reproduction of spectral line profiles and photometric evolution) are provided in Sections 2, 3, and 4 of the manuscript. To address the concern, we will revise the abstract to include a concise statement on the modeling approach and data sources. revision: yes

  2. Referee: [Abstract] Abstract: The central claim that comparability of inferred internal shock luminosity (from equatorial outflow model parameters) to warm WD pseudophotosphere luminosity confirms reprocessing origin depends on the SED model correctly decomposing the flared density-enhanced equatorial disk plus low-density bipolar regions, and on the shock luminosity being computed such that it can be directly compared without unaccounted geometric factors, reprocessing efficiency <1, or contributions from the WD itself or other components. The model also incorporates JHKL and UV data from the 2006/1985 events, which may not match 2021 conditions exactly.

    Authors: The decomposition is validated by the quality of the fits across all epochs and wavelengths, with the equatorial disk component required to match the IR excess and the bipolar components required for the UV/optical. Shock luminosity is computed from the dissipation of kinetic energy in the equatorial outflow using the fitted densities, velocities, and covering factors; geometric dilution and reprocessing are incorporated via the model solid angles, with efficiency near unity as the shocks directly heat the emitting gas. The WD pseudophotosphere is modeled as an independent component. Supplementary JHKL/UV data from prior outbursts are used only to supplement limited 2021 coverage in the earliest phases, with the paper noting the similarity of early evolution; we will add explicit discussion of these assumptions and any potential differences in the revised manuscript. revision: yes

Circularity Check

0 steps flagged

No circularity: claims rest on independent SED modeling of 2021 data

full rationale

The paper models the 2021 SED with optical spectroscopy and photometry, supplemented by prior-event data, to infer ejecta structure and shock luminosities. The comparability statement is an inference drawn from those fitted parameters rather than a quantity forced by construction or reduced to a self-citation. No step matches the enumerated circularity patterns; the central confirmation is presented as a consistency check against external observations, not an internal redefinition or fitted-input prediction. The derivation chain remains self-contained.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Insufficient information in the abstract to identify specific free parameters, axioms, or invented entities; the modeling is described only at the level of revealed structures and luminosity comparisons.

pith-pipeline@v0.9.1-grok · 5825 in / 1263 out tokens · 26289 ms · 2026-06-27T05:53:35.297230+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

242 extracted references · 181 canonical work pages · 59 internal anchors

  1. [1]

    2025, A&A, 695, A152, doi: 10.1051/0004-6361/202452447 18 Sokolovsky et al

    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

  2. [2]

    A., Ansoldi, S., Antonelli, L

    Proton acceleration in thermonuclear nova explosions revealed by gamma rays. Nature Astronomy , keywords =. doi:10.1038/s41550-022-01640-z , archivePrefix =. 2202.07681 , primaryClass =

    work page doi:10.1038/s41550-022-01640-z

  3. [3]

    , keywords =

    On the unidentified bands 6830-7088 in symbiotic stars. , keywords =. doi:10.1093/mnras/190.1.75 , adsurl =

    work page doi:10.1093/mnras/190.1.75

  4. [4]

    , year = 1974, month = jun, volume = 167, pages =

    Photometry of the eclipsing system AR Pavonis. , year = 1974, month = jun, volume = 167, pages =. doi:10.1093/mnras/167.3.635 , adsurl =

    work page doi:10.1093/mnras/167.3.635 1974

  5. [5]

    , year = 1979, month = apr, volume =

    Novalike Object in Vulpecula (Nova Vulpeculae 1979?). , year = 1979, month = apr, volume =

    1979

  6. [6]

    V., Chomiuk, L., et al

    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

  7. [7]

    , keywords =

    Multi-wavelength spectroscopic study of shock-driven phenomena in explosive outbursts in symbiotic-like recurrent novae with an emphasis on RS Ophiuchi. , keywords =. doi:10.1051/0004-6361/202245185 , archivePrefix =. 2303.07805 , primaryClass =

    work page doi:10.1051/0004-6361/202245185

  8. [8]

    title Galaxy Zoo: `Hanny's Voorwerp', a quasar light echo? journal volume 399 ( number 1 ): pages 129--140

    Near-infrared H- and K-band studies of the 2006 outburst of the recurrent nova RSOphiuchi. , keywords =. doi:10.1111/j.1365-2966.2009.15279.x , archivePrefix =. 0903.3794 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.15279.x 2006

  9. [9]

    Milliarcsecond N-Band Observations of the Nova RS Ophiuchi: First Science with the Keck Interferometer Nuller

    Milliarcsecond N-Band Observations of the Nova RS Ophiuchi: First Science with the Keck Interferometer Nuller. , keywords =. doi:10.1086/529422 , archivePrefix =. 0801.4165 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/529422

  10. [10]

    , eprint =

    A catalogue of symbiotic stars. , eprint =. doi:10.1051/aas:2000280 , adsurl =

    work page doi:10.1051/aas:2000280

  11. [11]

    , keywords =

    On the absence of symbiotic stars in globular clusters. , keywords =. doi:10.1093/mnras/staa1714 , archivePrefix =. 2004.05453 , primaryClass =

    work page doi:10.1093/mnras/staa1714 2004

  12. [12]

    Information Bulletin on Variable Stars , year = 1976, month = aug, volume =

    Observations of the Symbiotic Star CI Cyg in 1975. Information Bulletin on Variable Stars , year = 1976, month = aug, volume =

    1975

  13. [13]

    , year = 1991, month = apr, volume =

    Brightness Variation of the Cool Component of the Symbiotic Eclipsing Variable Ci-Cygni. , year = 1991, month = apr, volume =

    1991

  14. [14]

    Izvestiya Ordena Trudovogo Krasnogo Znameni Krymskoj Astrofizicheskoj Observatorii , year = 1992, month = jan, volume =

    The photometric observations of the symbiotic variables Z And, AG Peg and V443 HER in the eighties. Izvestiya Ordena Trudovogo Krasnogo Znameni Krymskoj Astrofizicheskoj Observatorii , year = 1992, month = jan, volume =

    1992

  15. [15]

    , keywords =

    AGB winds in interacting binary stars. , keywords =. doi:10.1093/mnras/staa403 , archivePrefix =. 2002.02570 , primaryClass =

    work page doi:10.1093/mnras/staa403 2002

  16. [16]

    , keywords =

    UBVRI photometry II: the Cousins VRI system, its temperature and absolute flux calibration, and relevance for two-dimensional photometry. , keywords =. doi:10.1086/130542 , adsurl =

    work page doi:10.1086/130542

  17. [17]

    , keywords =

    Equatorial Disk Formation around Rotating Stars Due to Ram Pressure Confinement by the Stellar Wind. , keywords =. doi:10.1086/172676 , adsurl =

    work page doi:10.1086/172676

  18. [18]

    An incisive look at the symbiotic star SS Leporis -- Milli-arcsecond imaging with PIONIER/VLTI

    An incisive look at the symbiotic star <ASTROBJ>SS Leporis</ASTROBJ>. Milli-arcsecond imaging with PIONIER/VLTI. , keywords =. doi:10.1051/0004-6361/201118036 , archivePrefix =. 1112.1514 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201118036

  19. [19]

    Hubble Space Telescope Imaging of the Expanding Nebular Remnant of the Recurrent Nova RS Ophiuchi (2006)

    Hubble Space Telescope Imaging of the Expanding Nebular Remnant of the 2006 Outburst of the Recurrent Nova RS Ophiuchi. , keywords =. doi:10.1086/520929 , archivePrefix =. 0706.2745 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/520929 2006

  20. [20]

    , year = 1947, month = jan, volume =

    The Electron Velocity Distribution in Gaseous Nebulae and Stellar Envelopes. , year = 1947, month = jan, volume =. doi:10.1086/144890 , adsurl =

    work page doi:10.1086/144890 1947

  21. [21]

    , year = 1944, month = jan, volume =

    On the mechanism of accretion by stars. , year = 1944, month = jan, volume =. doi:10.1093/mnras/104.5.273 , adsurl =

    work page doi:10.1093/mnras/104.5.273 1944

  22. [22]

    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

  23. [23]

    , year = 1966, month = oct, volume =

    The Continuous Spectrum of AG Pegasi. , year = 1966, month = oct, volume =

    1966

  24. [24]

    , keywords =

    The spectroscopic orbits and other parameters of the symbiotic binary FN Sgr. , keywords =. doi:10.1051/0004-6361:20042552 , adsurl =

    work page doi:10.1051/0004-6361:20042552

  25. [25]

    Spectroscopic orbits and variations of RS Oph

    Spectroscopic orbits and variations of RS Ophiuchi. , keywords =. doi:10.1051/0004-6361/200811417 , archivePrefix =. 0902.2177 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/200811417

  26. [26]

    , keywords =

    The variable light curve of the eclipsing symbiotic star AR Pavonis. , keywords =

  27. [27]

    Contributions of the Astronomical Observatory Skalnate Pleso , keywords =

    A description of the shellspec code. Contributions of the Astronomical Observatory Skalnate Pleso , keywords =

  28. [28]

    , keywords =

    The Relationship between Infrared, Optical, and Ultraviolet Extinction. , keywords =. doi:10.1086/167900 , adsurl =

    work page doi:10.1086/167900

  29. [29]

    , archivePrefix = "arXiv", eprint =

    Ionization structure of hot components in symbiotic binaries during active phases. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361/201219221 , adsurl =

    work page doi:10.1051/0004-6361/201219221

  30. [30]

    VLTI/AMBER interferometric observations of the recurrent Nova RS Oph 5.5 days after outburst

    AMBER/VLTI interferometric observations of the recurrent Nova RS Ophiuchii 5.5 days after outburst. , keywords =. doi:10.1051/0004-6361:20066609 , archivePrefix =. astro-ph/0611602 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20066609

  31. [31]

    C., Johnson, T

    Fermi LAT Gamma-ray Detection of the Recurrent Nova RS Ophiuchi during its 2021 Outburst. , keywords =. doi:10.3847/1538-4357/ac7eb7 , archivePrefix =. 2207.02921 , primaryClass =

    work page doi:10.3847/1538-4357/ac7eb7 2021

  32. [32]

    Binary orbits as the driver of gamma-ray emission and mass ejection in classical novae

    Binary orbits as the driver of -ray emission and mass ejection in classical novae. , keywords =. doi:10.1038/nature13773 , archivePrefix =. 1410.3473 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature13773

  33. [33]

    D., & Shen, K

    New Insights into Classical Novae. , keywords =. doi:10.1146/annurev-astro-112420-114502 , archivePrefix =. 2011.08751 , primaryClass =

    work page doi:10.1146/annurev-astro-112420-114502 2011

  34. [34]

    Information Bulletin on Variable Stars , keywords =

    Pulsating AGB star in the symbiotic nova PU Vulpeculae. Information Bulletin on Variable Stars , keywords =

  35. [35]

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

    A Wind analysis of an evolved Giant - FUSE and HST/STIS observations of an eclipsing Symbiotic Binary. 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun , year = 2005, editor =

    2005

  36. [36]

    An illumination effect and an eccentric orbit for the symbiotic binary PU Vul revealed by 32 years of optical spectroscopy

    An illumination effect and an eccentric orbit for the symbiotic binary PU Vul revealed by 32 yr of optical spectroscopy. , keywords =. doi:10.1093/mnras/sty1686 , archivePrefix =. 1802.10565 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty1686

  37. [37]

    , 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

  38. [38]

    Optical and IR Telescope Instrumentation and Detectors , year = 2000, editor =

    Design, construction, and performance of UVES, the echelle spectrograph for the UT2 Kueyen Telescope at the ESO Paranal Observatory. Optical and IR Telescope Instrumentation and Detectors , year = 2000, editor =. doi:10.1117/12.395512 , adsurl =

    work page doi:10.1117/12.395512 2000

  39. [39]

    , keywords =

    Evidence for Multiple Shocks from the -Ray Emission of RS Ophiuchi. , keywords =. doi:10.3847/1538-4357/acc105 , archivePrefix =. 2211.02059 , primaryClass =

    work page doi:10.3847/1538-4357/acc105

  40. [40]

    An IUE Survey of Interstellar H i Lyman-Alpha Absorption. II. Interpretations. , keywords =. doi:10.1086/174139 , adsurl =

    work page doi:10.1086/174139

  41. [41]

    Astronomy Letters , year = 2000, month = aug, volume =

    UBVRI Photometry of the Eclipsing Symbiotic System CI Cygni in 1996-1999. Astronomy Letters , year = 2000, month = aug, volume =. doi:10.1134/1.1306988 , adsurl =

    work page doi:10.1134/1.1306988 1996

  42. [42]

    Collimation and asymmetry of the hot blast wave from the recurrent nova V745 Scorpii

    Collimation and Asymmetry of the Hot Blast Wave from the Recurrent Nova V745 Sco. , keywords =. doi:10.3847/0004-637X/825/2/95 , archivePrefix =. 1604.04537 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/825/2/95

  43. [43]

    , year = 1998, month = apr, volume =

    Stellar radii of M giants. , year = 1998, month = apr, volume =. doi:10.1016/S1384-1076(98)00003-7 , adsurl =

    work page doi:10.1016/s1384-1076(98)00003-7 1998

  44. [44]

    , keywords =

    Circumstellar matter around M-giants in symbiotic binaries: SY MUSCAE and RW Hydrae. , keywords =

  45. [45]

    A Review of Bondi--Hoyle--Lyttleton Accretion

    A review of Bondi-Hoyle-Lyttleton accretion. , keywords =. doi:10.1016/j.newar.2004.06.001 , archivePrefix =. astro-ph/0406166 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.newar.2004.06.001 2004

  46. [46]

    The case of slowly accelerating oxygen-rich outflows

    Wind morphology around cool evolved stars in binaries. The case of slowly accelerating oxygen-rich outflows. , keywords =. doi:10.1051/0004-6361/202037492 , archivePrefix =. 2001.04482 , primaryClass =

    work page doi:10.1051/0004-6361/202037492 2001

  47. [47]

    Astronomy Letters , year = 2000, month = mar, volume =

    Evolution of the Symbiotic Star AS338 after Its Strong Outburst in 1983. Astronomy Letters , year = 2000, month = mar, volume =. doi:10.1134/1.20379 , adsurl =

    work page doi:10.1134/1.20379 1983

  48. [48]

    , keywords =

    Infrared observations of the 1985 outburst of RS Ophiuchi. , keywords =. doi:10.1093/mnras/234.3.755 , adsurl =

    work page doi:10.1093/mnras/234.3.755 1985

  49. [49]

    Infrared Spectroscopy of Symbiotic Stars. III. First Orbits for Three S-Type Systems. , keywords =. doi:10.1086/319966 , adsurl =

    work page doi:10.1086/319966

  50. [50]

    , keywords =

    The active phase of the hot component of Z Andromedae. , keywords =. doi:10.1086/175446 , adsurl =

    work page doi:10.1086/175446

  51. [51]

    I - Their progress and the expansion of the envelope

    A theory of hydrogen shell flashes on accreting white dwarfs. I - Their progress and the expansion of the envelope. II - The stable shell burning and the recurrence period of shell flashes. , keywords =. doi:10.1086/160029 , adsurl =

    work page doi:10.1086/160029

  52. [52]

    , year = 1982, month = jun, volume =

    A Theory of Hydrogen Shell Flashes on Accreting White Dwarfs - Part Two - the Stable Shell Burning and the Recurrence Period of Shell Flashes. , year = 1982, month = jun, volume =. doi:10.1086/160030 , adsurl =

    work page doi:10.1086/160030 1982

  53. [53]

    , keywords =

    AG Draconis observed with XMM-Newton. , keywords =. doi:10.1051/0004-6361:20078593 , adsurl =

    work page doi:10.1051/0004-6361:20078593

  54. [54]

    S and D'-Type Systems

    Light Curves of Symbiotic Stars in Massive Photometric Surveys II. S and D'-Type Systems. , keywords =

  55. [55]

    The Physics and Dynamics of Planetary Nebulae

  56. [56]

    A Prediction Formula of Supersoft X-ray Phase of Classical Novae

    A Prediction Formula of Supersoft X-ray Phase of Classical Novae. , keywords =. doi:10.1088/0004-637X/709/2/680 , archivePrefix =. 0912.1136 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/709/2/680

  57. [57]

    , keywords =

    Discovery of a nova super-remnant cavity surrounding RS Ophiuchi. , keywords =. doi:10.1093/mnrasl/slae016 , archivePrefix =. 2402.05855 , primaryClass =

    work page doi:10.1093/mnrasl/slae016

  58. [58]

    Astronomical photometry

  59. [59]

    Science , keywords =

    Time-resolved hadronic particle acceleration in the recurrent nova RS Ophiuchi. Science , keywords =. doi:10.1126/science.abn0567 , archivePrefix =. 2202.08201 , primaryClass =

    work page doi:10.1126/science.abn0567

  60. [60]

    Growing White Dwarfs to the Chandrasekhar Limit: The Parameter Space of the Single Degenerate SNIa Channel

    Growing White Dwarfs to the Chandrasekhar Limit: The Parameter Space of the Single Degenerate SNIa Channel. , keywords =. doi:10.3847/0004-637X/819/2/168 , archivePrefix =. 1508.03141 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/819/2/168

  61. [61]

    , keywords =

    Simulations of multiple nova eruptions induced by wind accretion in symbiotic systems. , keywords =. doi:10.1093/mnras/staa3600 , archivePrefix =. 2010.05869 , primaryClass =

    work page doi:10.1093/mnras/staa3600 2010

  62. [62]

    Infrared Spectroscopy of Symbiotic Stars. VII. Binary Orbit and Long Secondary Period Variability of CH Cygni. , keywords =. doi:10.1088/0004-637X/692/2/1360 , archivePrefix =. 0811.0631 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/692/2/1360

  63. [63]

    Infrared Spectroscopy of Symbiotic Stars. IX. D-type Symbiotic Novae. , keywords =. doi:10.1088/0004-637X/770/1/28 , adsurl =

    work page doi:10.1088/0004-637x/770/1/28

  64. [64]

    , keywords =

    Radio Observations of the 1985 Outburst of RS Ophiuchi. , keywords =. doi:10.1086/184687 , adsurl =

    work page doi:10.1086/184687 1985

  65. [65]

    , keywords =

    HST Eclipse Mapping of Dwarf Nova OY Carinae in Quiescence: an ``Fe II Curtain'' with Mach 6 Velocity Dispersion Veils the White Dwarf. , keywords =. doi:10.1086/174064 , adsurl =

    work page doi:10.1086/174064

  66. [66]

    Case B calculations for H I and He II

    Recombination-line intensities for hydrogenic ions - I. Case B calculations for H I and He II. , keywords =. doi:10.1093/mnras/224.3.801 , adsurl =

    work page doi:10.1093/mnras/224.3.801

  67. [67]

    Spectrum of the Yellow Symbiotic Star LT Delphini before, during, and after the 2017 Outburst

    Spectrum of the Yellow Symbiotic Star LT Delphini before, during, and after the 2017 Outburst. Astronomy Letters , keywords =. doi:10.1134/S1063773719040042 , archivePrefix =. 1904.11855 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1134/s1063773719040042 2017

  68. [68]

    , keywords =

    X-Rays from RS Ophiuchi's 2021 Eruption: Shocks In and Out of Ionization Equilibrium. , keywords =. doi:10.3847/1538-4357/ad1041 , archivePrefix =. 2311.17156 , primaryClass =

    work page doi:10.3847/1538-4357/ad1041 2021

  69. [69]

    , keywords =

    Eclipse cross-sections of cool components in double star systems. , keywords =

  70. [70]

    , keywords =

    Orbital Elements of the Symbiotic Star Z Andromedae from Optical Linear Polarization During the Quiescent Phase. , keywords =. doi:10.1088/0004-6256/140/1/235 , adsurl =

    work page doi:10.1088/0004-6256/140/1/235

  71. [71]

    Harvard College Observatory Bulletin , year = 1941, month = jun, volume = 915, pages =

    Notes on Variable Stars. Harvard College Observatory Bulletin , year = 1941, month = jun, volume = 915, pages =

    1941

  72. [72]

    Contributions of the Astronomical Observatory Skalnate Pleso , keywords =

    Insights from mid-infrared interferometric observations of the symbiotic nova RS Ophiuchi. Contributions of the Astronomical Observatory Skalnate Pleso , keywords =. doi:10.31577/caosp.2025.55.3.98 , adsurl =

    work page doi:10.31577/caosp.2025.55.3.98 2025

  73. [73]

    1994, ApJ, 437, 802, doi: 10.1086/175041 —

    Optically Thick Winds in Nova Outbursts. Astrophys. J. , keywords =. doi:10.1086/175041 , adsurl =

    work page doi:10.1086/175041

  74. [74]

    Evolution of the Symbiotic Nova PU Vul -- Outbursting White Dwarf, Nebulae, and Pulsating Red Giant Companion

    Evolution of the Symbiotic Nova PU Vul Outbursting White Dwarf, Nebulae, and Pulsating Red Giant Companion. , keywords =. doi:10.1088/0004-637X/750/1/5 , archivePrefix =. 1202.6171 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/750/1/5

  75. [75]

    X-Ray Flashes in Recurrent Novae: M31N 2008-12a and the Implications of the Swift Non-detection

    X-ray Flashes in Recurrent Novae: M31N 2008-12a and the Implications of the Swift Nondetection. , keywords =. doi:10.3847/0004-637X/830/1/40 , archivePrefix =. 1607.07985 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/830/1/40 2008

  76. [76]

    A Self-Consistent Model for a Full Cycle of Recurrent Novae -- Wind Mass Loss Rate and X-Ray Luminosity

    A Self-consistent Model for a Full Cycle of Recurrent Novae Wind Mass-Loss Rate and X-Ray Luminosity. , keywords =. doi:10.3847/1538-4357/838/2/153 , archivePrefix =. 1701.01825 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/838/2/153

  77. [77]

    , keywords =

    Physics of nova outbursts: A theoretical model of classical nova outbursts with self-consistent wind mass loss. , keywords =. doi:10.1093/pasj/psac051 , archivePrefix =. 2206.03136 , primaryClass =

    work page doi:10.1093/pasj/psac051

  78. [78]

    , keywords =

    A Light-curve Analysis of the X-Ray Flash First Observed in Classical Novae. , keywords =. doi:10.3847/2041-8213/ac85c1 , archivePrefix =. 2208.01249 , primaryClass =

    work page doi:10.3847/2041-8213/ac85c1 2041

  79. [79]

    , keywords =

    The orbital period of the symbiotic star AX Per. , keywords =. doi:10.1086/130957 , adsurl =

    work page doi:10.1086/130957

  80. [80]

    Cambridge and New York, Cambridge University Press, 1986, 295 p

    The symbiotic stars. Cambridge and New York, Cambridge University Press, 1986, 295 p. , year = 1986, adsurl =

    1986

Showing first 80 references.