Pith. sign in

REVIEW 3 major objections 4 minor 1 cited by

A 70 pc-Diameter Nova Super-remnant Surrounding the Recurrent Nova RS Ophiuchi

T0 review · 3 major / 4 minor · reviewed 2026-08-15 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read Deep narrowband imaging and follow-up spectroscopy reveal a roughly 70-parsec, possibly bi-lobed shell of shocked, low-density gas around the recurrent nova RS Ophiuchi, which the authors identify as a nova super-remnant built by…

desk verdict A promising but not yet secure 70-pc nova super-remnant candidate around RS Oph; the association needs a control field or independent distance/velocity tie before it is accepted. read the letter →

arxiv 2505.09510 v1 pith:ZZW4W2HI submitted 2025-05-14 astro-ph.SR astro-ph.GAastro-ph.HE

Michael M. Shara , Kenneth M. Lanzetta , Alexandra Masegian , James T. Garland , Stefan Gromoll , Alexei Kniazev , Lee Townsend , David Zurek
show 4 more authors
Joanna Mikolajewska David Valls-Gabaud Frederick M. Walter John K. Webb
This is my paper · ORCID
classification astro-ph.SRastro-ph.GAastro-ph.HE
keywords recurrentnovaenovasuper-remnantRSOphiuchicataclysmicvariablesbinaries:closestars:windsandoutflowsinterstellarmedium
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

The paper reports the discovery of a faint, roughly 1.5-degree-wide (about 70 parsec) shell of line emission around the recurrent nova RS Ophiuchi, a binary system that erupts every decade or two. The authors interpret this shell as a nova super-remnant, a structure built over tens of millennia as the fastest material from each new eruption overtakes and piles up against slower ejecta from earlier eruptions and swept-up interstellar gas. If they are right, RS Ophiuchi becomes only the third Galactic recurrent nova known to host such a super-remnant, and the result strengthens the prediction that every recurrent nova is surrounded by one. The shell's extremely low surface brightness and very large angular size also explain why such super-remnants have been so difficult to find.

What carries the argument

The central object is the nova super-remnant (NSR), a parsec-to-hundreds-of-parsec shell formed when fast ejecta from each recurrent-nova eruption overtake and collide with slower ejecta and swept-up interstellar material from previous eruptions, so that thousands of individual shells pile up into one expanding structure. The observational signature that carries the detection is faint line emission in H-alpha, [NII], and [SII] at low expansion velocities of a few tens of km/s, with shock-ionization line ratios and no high-velocity or high-ionization tracers such as [OIII]. The key instrumental step is wide-field narrowband-minus-continuum difference imaging, which isolates line emission at surface brightness levels far below what ordinary images show, followed by long-slit spectroscopy to measure velocities, line ratios, and the [SII] doublet ratio used to estimate density and mass.

What would settle it

Observe a control field at the same Galactic latitude with the same narrowband filters and slit geometry: if comparable H-alpha, [NII], and [SII] surface brightness appears there, or if a 21-centimeter neutral-hydrogen map shows no coherent shell expanding at tens of km/s centered on RS Ophiuchi, the nebulosity is unrelated interstellar gas rather than a nova super-remnant.

Watch

Extended reading notes

Core claim

At the parallax distance of 2.68 ± 0.16 kiloparsec, the roughly 1.5-degree structure has a diameter of about 70 parsec, more than two orders of magnitude larger than the arcsecond-scale ejecta seen around RS Oph in modern eruptions. The emission appears in H-alpha, [NII], and [SII] difference images but not in [OIII], HeI, or HeII; the logarithmic [NII]/H-alpha and [SII]/H-alpha ratios are both about -0.45, a signature of shock ionization, and the [SII] 6716/6731 ratio of 1.41 ± 0.05 implies an electron density below roughly 50 electrons per cubic centimeter. The H-alpha line of the outer shell sits near -14 km/s, close to the -38.7 km/s systemic velocity, with no high-velocity components. The authors therefore rule out a supernova remnant or planetary nebula and model the nebula as a mostly hollow 35-parsec-radius shell with a 3.5-parsec-thick boundary layer, which yields a mass of about 20 to 200 solar masses, an expansion speed of a few tens of km/s, and an age of order 50 to 100 thousand years.

Load-bearing premise

The extended H-alpha, [NII], and [SII] emission is assumed to be physically associated with RS Ophiuchi at 2.68 kiloparsec, rather than unrelated diffuse interstellar gas lying in the same direction on the sky, an assumption the paper does not test with a control field or an independent velocity or distance tie.

Editorial extensions

If this is right

  • RS Ophiuchi becomes the third Galactic recurrent nova known to host a nova super-remnant, after KT Eri and T CrB, and the fourth such super-remnant known overall.
  • The implied age of 50 to 100 thousand years means the RS Oph white dwarf has erupted thousands of times, far more than the eight eruptions recorded since 1898, and future eruptions will continue to run into this massive shell.
  • The shell's extremely low surface brightness and roughly 1.5-degree angular extent explain why previous searches missed it, and they argue that similarly deep narrowband surveys are the way to find super-remnants around the remaining Galactic recurrent novae.
  • The absence of [OIII] and of high-velocity gas rules out a supernova remnant or planetary nebula as the origin of the nebulosity, leaving the nova-built shell as the viable interpretation.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • Beyond the paper: applying the same difference-imaging technique to the remaining eight Galactic recurrent novae would test whether super-remnants are truly universal, as predicted, and would show how many eruptive cycles are needed to build a detectable shell.
  • Beyond the paper: the roughly bi-lobed shape, with a linear southern boundary nearly perpendicular to RS Oph's proper motion of about 6 milliarcseconds per year, suggests the nova's motion through the interstellar medium is snow-plowing material; comparing the surface brightness on the leading and trailing sides would test this picture.
  • Beyond the paper: mapping the full H-alpha velocity field across the 1.5-degree shell would show whether the outer-shell velocity of -14 km/s is part of a coherent expansion around the systemic velocity or reveals contamination by unrelated interstellar gas, directly testing the physical association.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 4 minor

Summary. The paper reports deep narrowband imaging with the Condor Array Telescope and follow-up SALT spectroscopy of a ~1.5-degree, ~70 pc-sized nebulosity around the recurrent nova RS Oph. The authors interpret this structure as a nova super-remnant (NSR) built up by thousands of eruptions over ~50-100 kyr, with a shell mass of ~20-200 solar masses, an expansion velocity of a few tens of km/s, and shock-like line ratios. The detection is presented as support for the theoretical prediction that all recurrent novae possess such structures. The observational material includes H-alpha, [NII], and [SII] images and spectra, a [SII] 6716/6731 density-sensitive ratio, and radial velocities of the outer shell.

Significance. If the association with RS Oph is correct, this would be a significant addition to the short list of known nova super-remnants, and it would strengthen the case that such structures are ubiquitous around recurrent novae. The paper's strengths include very deep imaging with careful sky subtraction, explicit discussion of the low-surface-brightness selection effect, and the use of diagnostic line ratios and the [SII] doublet ratio. The authors also state clearly where their mass estimate depends on assumptions. However, the central claim currently rests on the physical association of diffuse Galactic emission with RS Oph, and that association is not independently tested. The reported surface brightness and line ratios are also consistent with the Galactic warm ionized medium, so the identification as an NSR remains conditional rather than demonstrated.

major comments (3)
  1. [Section 3.1 and Section 5.1] The central claim that the ~1.5-degree nebulosity is a physical shell around RS Oph at 2.68 kpc is not tested against the most plausible alternative: unrelated diffuse Galactic interstellar gas along the same line of sight. No control field is presented, and because the structure fills most of the 2.2 x 1.5 degree Condor field, there is no on-image blank-sky baseline. The surface brightness (~1.4 x 10^-17 erg s^-1 cm^-2 arcsec^-2) and the line ratios log([NII]/H-alpha) ~ log([SII]/H-alpha) ~ -0.45 (Figure 11) are characteristic of the warm ionized medium, not uniquely of shock-ionized nova ejecta. An independent distance or velocity tracer, such as H I 21-cm data, dust extinction mapping, or proper motion of the shell, is needed to break this degeneracy.
  2. [Section 4.2, Figure 11] The only kinematic datum for the outer shell is a heliocentric H-alpha velocity of ~ -14.3 km/s, which differs from the RS Oph systemic velocity of -38.7 +/- 0.4 km/s by about 25 km/s. The paper attributes this offset to deceleration of the ejecta by swept-up ISM (Section 4.2), but this is an untested interpretation. If the emission were instead diffuse Galactic gas, its velocity would not be expected to match the systemic velocity of RS Oph. A quantitative model of the expected velocity field of a decelerating NSR, or a measurement of the velocity gradient across the shell, would be needed to support the association.
  3. [Section 5.2] The shell mass estimate of 20-200 solar masses is explicitly conditional on the assumption that the [SII] lines arise in gas associated with the NSR, as stated in the text. The estimate also adopts a shell geometry (radius 35 pc, thickness 3.5 pc), a density range of 5-50 H atoms/cm^3, and an age of 40,000 years, each of which is only roughly constrained. The subsequent 'sanity check' reuses the assumed age and expansion velocity, so it does not provide independent validation. This is acceptable as a rough estimate if the association is established, but it cannot by itself corroborate the NSR interpretation.
minor comments (4)
  1. [Table 1] The [NII] observation row lists a start date of 2024-06-04 and an end date of 2024-05-30, which is internally inconsistent; the dates should be checked and corrected.
  2. [Figure 1 caption] The caption contains a typographical error: '[NII]]' has a double closing bracket.
  3. [Section 2.1] The sentence 'The dates of observation and reaches of the images of T CrB are presented in Table 1' should refer to RS Oph, not T CrB.
  4. [Figure 11] The middle panel reports an unresolved H-alpha line with FWHM ~15 km/s, but the plot axis is labeled 'sigma_gas' and shows values from 10 to 40 km/s; the relation between the plotted quantity and the stated FWHM should be clarified.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the RS Oph nebulosity detection is observational, and the theoretical NSR framework is an independently cited model rather than an input of the derivation.

full rationale

The paper's central claim is a new observational detection of extended H-alpha/[NII]/[SII] emission around RS Oph. The identification as a nova super-remnant rests on the independent hydrodynamic model of Healy-Kalesh et al. (2023), which is cited as external theory and is not fitted to the RS Oph data. The mass and age estimates in Sections 5.1-5.2 are explicitly rough and conditional ('assuming, of course, that the [SII] lines ... arise in gas associated with the NSR'), and the sanity check reuses the assumed age and expansion speed, but this is a self-consistency estimate, not a prediction derived from first principles. Previous detections by the same group (KT Eri, T CrB) are used only as motivation, not as load-bearing evidence. The absence of a control field and the roughly 25 km/s velocity offset between the outer shell and RS Oph's systemic velocity are important correctness and interpretation risks, but they concern whether the emission is physically associated with RS Oph, not whether any claimed derivation reduces to its inputs by construction. No equation in the paper defines one claimed result in terms of another, and no fitted parameter is renamed as a prediction. Hence no circularity.

Assumptions & free parameters 5 free parameters · 5 assumptions · 0 invented entities

The paper's central claim rests on an association between faint extended H-alpha emission and RS Oph; this assumption is flagged only inside the mass estimate. The derived physical parameters, density, geometry, and age, are rough and model dependent. No new physical entities are introduced.

free parameters (5)
  • NSR electron density = 5 to 50 H atoms per cubic cm
    The [SII] 6716/6731 ratio of about 1.41 gives only an upper limit near 50 electrons per cubic cm in the low-density limit; the lower bound of 5 is chosen ad hoc. The shell mass scales linearly with this density (Section 5.2).
  • Shell geometry (radius and thickness) = 35 pc radius, 3.5 pc boundary thickness
    A spherical shell with boundary thickness 10 percent of the radius is assumed, following Healy-Kalesh et al. 2023 simulations; it is not measured for RS Oph.
  • Expansion velocity for the mass sanity check = about 50 km/s
    The paper speaks of 'a few tens of km/s' and uses about 50 km/s in the energy argument of Section 5.2, while observed values range from about -14 to +60 km/s.
  • NSR age = 50 to 100 kyr
    Inferred from proper motion, initial ejecta speeds, and assumed deceleration; not directly measured from, for example, an expansion parallax.
  • Number of eruptions = about 2000 over 40,000 years
    Adopted in the energy budget of Section 5.2 and based on the current accretion rate and the observed roughly two-decade recurrence interval.
assumptions (5)
  • domain assumption RS Oph is at the Gaia distance of 2.68 +/- 0.16 kpc (Schaefer 2022).
    The angular size of the shell is converted to 70 pc using this distance in Section 5.1.
  • domain assumption Recurrent nova eruptions build NSRs via shell pile-up, as modeled by Healy-Kalesh et al. 2023.
    The interpretation of the nebula as a nova super-remnant relies on this theoretical framework in Sections 1.2, 4.2, and 6.
  • ad hoc to paper The detected H-alpha, [NII], and [SII] emission lies at the distance of RS Oph and is not foreground or background Galactic gas.
    Stated as an assumption in Section 5.2 for the mass estimate; no independent distance or velocity tie is provided.
  • domain assumption The Luminance image provides a valid continuum subtraction for the narrowband difference images.
    The difference-image method in Section 3.1 assumes line emission losses are negligible because of the broad L-band response.
  • standard math The low-density limit of the [SII] 6716/6731 doublet applies to the observed gas.
    Used in Section 4.2 to convert the ratio 1.41 +/- 0.05 into an electron density upper limit of roughly 50 electrons per cubic cm.

how reviews work

0 comments
Cite this review

Pith. "Pith review of A 70 pc-Diameter Nova Super-remnant Surrounding the Recurrent Nova RS Ophiuchi." pith.science (2026). https://pith.science/paper/ZZW4W2HI

@misc{pith2026250509510,
  author       = {Pith},
  title        = {Pith review of: A 70 pc-Diameter Nova Super-remnant Surrounding the Recurrent Nova RS Ophiuchi},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/ZZW4W2HI}},
  note         = {Machine review of arXiv:2505.09510}
}
read the original abstract

Recurrent novae undergo thermonuclear-powered eruptions separated by less than 100 years, enabled by subgiant or red giant donors transferring hydrogen-rich matter at very high rates onto their massive white dwarf companions. The most-rapidly moving parts of envelopes ejected in successive recurrent nova events are predicted to overtake and collide with the slowest ejecta of the previous eruption, leading to the buildup of vast (~ 10 - 100 parsec) super-remnants surrounding all recurrent novae; but only three examples are currently known. We report deep narrowband imaging and spectroscopy which has revealed a ~ 70-parsec-diameter shell surrounding the frequently recurring nova RS Ophiuchi. We estimate the super-remnant mass to be ~ 20 - 200 solar masses, expanding at a few tens of km/s, with an age of order 50-100 kyr. Its extremely low surface brightness and large angular size help explain the hitherto surprising absence of nova super-remnants. Our results support the prediction that ALL recurrent novae are surrounded by similar extended structures.

Figures

Figures reproduced from arXiv: 2505.09510 by the authors.

Figure 1
Figure 1. Condor narrowband images of the area surrounding RS Oph in HeII, [OIII], HeI, H α, [NII]] and [SII] filters. RS Oph is marked with red ticks. Images have been 8x8 block-summed and are displayed with linear scaling. The RS Oph nova super-remnant is immediately apparent only in the H α image as a nebulosity filling much of the field-of-view, and bounded by a nearly-one-degree long linear feature running NE to SW at th… view at source ↗
Figure 2
Figure 2. Difference images (narrowband minus Luminance) of the area surrounding RS Oph. Images have been 8x8 block￾summed and are displayed with linear scaling. RS Oph is marked with red ticks. The nova super-remnant is now apparent in the H α, [NII]] and [SII] filters. 4.1. Slit locations As noted in Section 2, three spectra (each of one hour duration) of the RS Oph nebula were taken with SALT. The three slit placements are… view at source ↗
Figure 3
Figure 3. Hα - Luminance difference image of RS Oph NSR (same as in [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figures from the paper (9 more)
Figure 4
Figure 4. Figure 4: RGB image of RS Oph (position indicated with red ticks) and its surrounding emission. Each of the three channels is a block-summed difference image (see [PITH_FULL_IMAGE:figures/full_fig_p008_4.png]
Figure 5
Figure 5. Figure 5: Same as [PITH_FULL_IMAGE:figures/full_fig_p009_5.png]
Figure 6
Figure 6. Figure 6: Hα image of the region surrounding RS Oph, which is indicated by diagonal red ticks. The proper motion of RS Oph (with a Gaia-measured amplitude of 6.11 mas/yr) is shown as a white arrow, whose length corresponds to the motion of RS Oph in the past 50 kyr. The position…
Figure 7
Figure 7. Figure 7: SALT spectrum of the inner RS Oph shell taken on 10 August 2023 with the magenta colored slit of [PITH_FULL_IMAGE:figures/full_fig_p011_7.png]
Figure 8
Figure 8. Figure 8: Top: Same as [PITH_FULL_IMAGE:figures/full_fig_p012_8.png]
Figure 9
Figure 9. Figure 9: SALT spectrum of the outer RS shell shell, taken with the cyan-colored slit of [PITH_FULL_IMAGE:figures/full_fig_p013_9.png]
Figure 10
Figure 10. Figure 10: Same as [PITH_FULL_IMAGE:figures/full_fig_p013_10.png]
Figure 11
Figure 11. Figure 11: Top: Measured radial velocity of the Hα line along the extent of the Northern (cyan-colored) slit. Data were binned into 10 arcsec-wide bins to reduce noise. The velocity of each binned data point was determined relative to the nearest night sky line at 655.35515 nm. …
Figure 12
Figure 12. Figure 12: The ratio of the forbidden [SII] line doublet 6716/6731 along the cyan-colored, “outer” shell SALT slit seen in [PITH_FULL_IMAGE:figures/full_fig_p015_12.png]

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. X-rays from shock-heated gas in recurrent-nova remnants: Nested nova shells in a structured circumstellar medium

    astro-ph.HE 2026-08 conditional novelty 6.0 of 10

    A 3D simulation of nine repeated nova eruptions shows that nested shell collisions produce a slowly fading soft X-ray component and episodic hard X-ray flares, roughly matching the extended X-rays seen around RS Ophiuchi.

Reference graph

Works this paper leans on

33 extracted references · 11 canonical work pages · cited by 1 Pith paper

  1. [1]

    A., Ansoldi, S., Antonelli, L

    Acciari, V. A., Ansoldi, S., Antonelli, L. A., et al. 2022, Nature Astronomy, 6, 689, doi: 10.1038/s41550-022-01640-z

    doi:10.1038/s41550-022-01640-z 2022

  2. [2]

    Michalitisianos, A. G. 1983, ApJS, 53, 573, doi: 10.1086/190902

    work page doi:10.1086/190902 1983

  3. [3]

    F., Harman, D

    Bode, M. F., Harman, D. J., O’Brien, T. J., et al. 2007, ApJL, 665, L63, doi: 10.1086/520929

    doi:10.1086/520929 2007

  4. [4]

    F., & Kahn, F

    Bode, M. F., & Kahn, F. D. 1985, MNRAS, 217, 205, doi: 10.1093/mnras/217.1.205

    doi:10.1093/mnras/217.1.205 1985

  5. [5]

    A., Mohamed, S., & Podsiadlowski, P

    Booth, R. A., Mohamed, S., & Podsiadlowski, P. 2016, MNRAS, 457, 822, doi: 10.1093/mnras/stw001

    doi:10.1093/mnras/stw001 2016

  6. [6]

    E., & Garc´ ıa, L

    Brandi, E., Quiroga, C., Miko lajewska, J., Ferrer, O. E., & Garc´ ıa, L. G. 2009, A&A, 497, 815, doi: 10.1051/0004-6361/200811417

    doi:10.1051/0004-6361/200811417 2009

  7. [7]

    J., Hounsell, R., O’Brien, T

    Darnley, M. J., Hounsell, R., O’Brien, T. J., et al. 2019, Nature, 565, 460, doi: 10.1038/s41586-018-0825-4

    doi:10.1038/s41586-018-0825-4 2019

  8. [8]

    J., Proga, D., Mikolajewska, J., & Wade, R

    Dobrzycka, D., Kenyon, S. J., Proga, D., Mikolajewska, J., & Wade, R. A. 1996, AJ, 111, 2090, doi: 10.1086/117945

    doi:10.1086/117945 1996

Show all 33 references
  1. [9]

    Duerbeck, H. W. 1987, Ap&SS, 131, 461, doi: 10.1007/BF00668126

    1987 doi

  2. [10]

    M., Albinson, J

    Evans, A., Callus, C. M., Albinson, J. S., et al. 1988, MNRAS, 234, 755, doi: 10.1093/mnras/234.3.755

    1988 doi

  3. [11]

    Ford, H. C. 1978, ApJ, 219, 595, doi: 10.1086/155819 H. E. S. S. Collaboration, Aharonian, F., Ait Benkhali, F., et al. 2022, Science, 376, 77, doi: 10.1126/science.abn0567

    1978 doi

  4. [12]

    W., Darnley, M

    Healy-Kalesh, M. W., Darnley, M. J., Harvey, ´E. J., et al. 2023, MNRAS, 521, 3004, doi: 10.1093/mnras/stad617

    2023 doi

  5. [13]

    Newsam, A. M. 2024a, MNRAS, 529, L175, doi: 10.1093/mnrasl/slae016

    doi

  6. [14]

    W., Darnley, M

    Healy-Kalesh, M. W., Darnley, M. J., & Shara, M. M. 2024b, MNRAS, 528, 3531, doi: 10.1093/mnras/stae251

    doi

  7. [15]

    Hillman, Y., Prialnik, D., Kovetz, A., & Shara, M. M. 2016, ApJ, 819, 168, doi: 10.3847/0004-637X/819/2/168

    2016 doi

  8. [16]

    M., Prialnik, D., & Kovetz, A

    Hillman, Y., Shara, M. M., Prialnik, D., & Kovetz, A. 2020, Nature Astronomy, 4, 886, doi: 10.1038/s41550-020-1062-y

    2020 doi

  9. [17]

    M., van Gorkom, J

    Hjellming, R. M., van Gorkom, J. H., Taylor, A. R., et al. 1986, ApJL, 305, L71, doi: 10.1086/184687

    1986 doi

  10. [18]

    Kniazev, A. V. 2022, Astrophysical Bulletin, 77, 334, doi: 10.1134/S1990341322030075

    2022 doi

  11. [19]

    Y., Pustilnik, S

    Kniazev, A. Y., Pustilnik, S. A., & Zucker, D. B. 2008, MNRAS, 384, 1045, doi: 10.1111/j.1365-2966.2007.12540.x

    2008

  12. [20]

    A., Nordsieck, K

    Kobulnicky, H. A., Nordsieck, K. H., Burgh, E. B., et al. 2003, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 4841, Instrument Design and Performance for Optical/Infrared Ground-based Telescopes, ed. M. Iye & A. F. M. Moorwood, 1634–1644,...

    2003 doi

  13. [21]

    M., Gromoll, S., Shara, M

    Lanzetta, K. M., Gromoll, S., Shara, M. M., et al. 2023, PASP, 135, 015002, doi: 10.1088/1538-3873/acaee6 Le Tiran, L., Lehnert, M. D., van Driel, W., Nesvadba, N. P. H., & Di Matteo, P. 2011, A&A, 534, L4, doi: 10.1051/0004-6361/201117609 Miko lajewska, J., & Shara, M. M. 201...

    2023

  14. [22]

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

    1967

  15. [23]

    M., & Shaviv, G

    Prialnik, D., Shara, M. M., & Shaviv, G. 1978, A&A, 62, 339 —. 1979, A&A, 72, 192 Santamar´ ıa, E., Guerrero, M. A., Ramos-Larios, G., et al. 2020, ApJ, 892, 60, doi: 10.3847/1538-4357/ab76c5

    1978 doi

  16. [24]

    Schaefer, B. E. 2010, ApJS, 187, 275, doi: 10.1088/0067-0049/187/2/275 —. 2022, MNRAS, 517, 6150, doi: 10.1093/mnras/stac2900

    2010 doi

  17. [25]

    M., Zurek, D., Schaefer, B

    Shara, M. M., Zurek, D., Schaefer, B. E., et al. 2015, ApJ, 805, 148, doi: 10.1088/0004-637X/805/2/148

    2015 doi

  18. [26]

    M., Lanzetta, K

    Shara, M. M., Lanzetta, K. M., Garland, J. T., et al. 2024a, MNRAS, 529, 224, doi: 10.1093/mnras/stad3612

    doi

  19. [27]

    M., Lanzetta, K

    Shara, M. M., Lanzetta, K. M., Masegian, A., et al. 2024b, ApJL, 977, L48, doi: 10.3847/2041-8213/ad991e

    doi

  20. [28]

    M., Lanzetta, K

    Shara, M. M., Lanzetta, K. M., Garland, J. T., et al. 2024c, MNRAS, 529, 212, doi: 10.1093/mnras/stad3220

    doi

  21. [29]

    N., Kenyon, S

    Shore, S. N., Kenyon, S. J., Starrfield, S., & Sonneborn, G. 1996, ApJ, 456, 717, doi: 10.1086/176692

    1996 doi

  22. [30]

    L., Luna, G

    Sokoloski, J. L., Luna, G. J. M., Mukai, K., & Kenyon, S. J. 2006, Nature, 442, 276, doi: 10.1038/nature04893

    2006 doi

  23. [31]

    W., Sparks, W

    Starrfield, S., Truran, J. W., Sparks, W. M., & Kutter, G. S. 1972, ApJ, 176, 169, doi: 10.1086/151619 18 Shara, Lanzetta, Masegian et al

    1972 doi

  24. [32]

    A., Tomova, M

    Tomov, N. A., Tomova, M. T., Stoyanov, K. A., et al. 2023, A&A, 671, A49, doi: 10.1051/0004-6361/202243068

    2023 doi

  25. [33]

    M., & Kovetz, A

    Yaron, O., Prialnik, D., Shara, M. M., & Kovetz, A. 2005, ApJ, 623, 398, doi: 10.1086/428435

    2005 doi

Pith tools

Reviewed August 15, 2026 · model on record in the stance chip above.