Critical comments on publications by S. Hoffmann and N. Vogt on historical novae/supernovae and their candidates

Neuhäuser, R.; Neuhäuser, Dagmar L.

doi:10.1002/asna.202113872

Cited by 4 publications

(2 citation statements)

References 49 publications

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“…The best study of the Chinese records of SN 1181 is certainly the long and detailed chapter in SG2002, with this being authoritative and definitive. The most recent discussion of these same Chinese records appears in Ritter et al (2021), which unfortunately adopted most of its discussions and results from the thoroughly discredited source of Hoffman, Vogt, & Protte (2020), which has a high rate of bad errors of many kinds (Neuhäuser & Neuhäuser 2021). With this situation and with the new information on Pa 30 and supernovae, it is worthwhile re-examining the original Chinese and Japanese reports.…”

Section: The Ancient Chinese and Japanese Datamentioning

confidence: 99%

The Path from the Chinese and Japanese Observations of Supernova 1181 AD, to a Type Iax Supernova, to the Merger of CO and ONe White Dwarfs

Schaefer¹

2023

Preprint

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In 1181 AD, Chinese and Japanese observers reported a bright 'Guest Star' in the constellation Chuanshe, unmoving and visible for 185 days. In 2013, D. Patchick discovered a unique nebula surrounding a unique star, with two groups attributing this structure, named 'Pa 30', to be the supernova remnant of SN 1181, as a sub-subclass of supernova, the low-luminosity Type Iax. Here, I provide a wide range of new observational evidence: First, a detailed analysis of the original Chinese and Japanese reports places the 'Guest Star' of 1181 into a small region with the only interesting source being Pa 30. Second, the ancient records confidently place the peak magnitude as 0.0>𝑉 peak >−1.4, and hence peak absolute magnitude of −14.5>𝑀 V,peak >−16.0 mag. Third, the Pa 30 central star is fading from 𝐵=14.90 in 1917, to 𝐵=16.20 in 1950, to 𝐵=16.58 in 2022. Fourth, recent light curves show typical variability with full-amplitude of 0.24 mag on time-scales of one day and longer, critically with no coherent modulations for periods from 0.00046-10 days to strict limits. Fifth, the spectral energy distribution from the far-infrared to the ultraviolet is a nearly perfect power-law with 𝐹 𝜈 ∝ 𝜈 0.99±0.07 , observed luminosity of 128±24 L , and absolute magnitude 𝑀 V =+1.07. I collect my new evidences with literature results to make a confident case to connect the Oriental observations to a supernova, then to Pa 30, then to a low-luminosity Type Iax SN, then to the only possible explosion mechanism as a merger between CO and ONe white dwarfs.

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Section: The Ancient Chinese and Japanese Datamentioning

confidence: 99%

The Path from the Chinese and Japanese Observations of Supernova 1181 AD, to a Type Iax Supernova, to the Merger of CO and ONe White Dwarfs

Schaefer¹

2023

Preprint

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“…However, the discovery of a faint and transient event might be difficult. For this,

{m}_{\mathrm{V}}\lesssim

1–3 has been often assumed previously (e.g., Clark & Stephenson 1977; Hertzog 1986; Neuhäuser & Neuhäuser 2021; Stephenson & Green 2009). To increase the number of possible candidates, we assume that unaided observers could catch an event with an apparent magnitude of 3.…”

Section: Association Of the Events With Remnants Of Astrophysical Tra...mentioning

confidence: 84%

A list of guest‐star records in Korean history and their possible counterparts

Park

Jeon

2022

Astron Nachr

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We report on guest-star events recorded in Korean history in the period between A.D. 154 and 1807. We search five books, namely Joseonwangjosillok, Seungjeongwonilgi, Jeungbomoonheonbigo, Goryeosa, and Samguksagi for "guest star" and find 37 events. Seventeen of the guest stars are almost certainly comets as identified previously and are not astrophysical transient events of our interest; we list them for completeness but do not discuss them in detail. We review the historical recordings and the previous interpretations of the guest-star events and scrutinize them in order to better identify the guest stars. We infer the positions of 11 events and compare them to astrophysical objects in up-to-date catalogues of possible remnants of transient events: supernova remnants, pulsars, magnetars, novae, and cataclysmic variables. We consider the positions and visibility of the astrophysical events, select possible counterparts, and present a list of them for the guest stars with an inferred position.

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Introducing the Condor Array Telescope – III. The expansion and age of the shell of the dwarf nova Z Camelopardalis, and detection of a second, larger shell

Shara,

Lanzetta,

Garland

et al. 2024

Monthly Notices of the Royal Astronomical Society

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The existence of a vast nova shell surrounding the prototypical dwarf nova Z Camelopardalis (Z Cam) proves that some old novae undergo metamorphosis to appear as dwarf novae thousands of years after a nova eruption. The expansion rates of ancient nova shells offer a way to constrain both the time between nova eruptions and the time for post-nova mass transfer rates to decrease significantly, simultaneously testing nova thermonuclear runaway models and hibernation theory. Previous limits on the expansion rate of part of the Z Cam shell constrain the inter-eruption time between Z Cam nova events to be >1300 yr. Deeper narrow-band imaging of the ejecta of Z Cam with the Condor Array Telescope now reveals very low surface brightness areas of the remainder of the shell. A second, even fainter shell is also detected, concentric with and nearly three times the size of the ‘inner’ shell. This is the first observational support of the prediction that concentric shells must surround the frequently erupting novae of relatively massive white dwarfs. The Condor images extend our Z Cam imaging baseline to 15 yr, yielding the inner shell’s expansion rate as v = 83 ± 37 km s−1 at 23 deg south of west, in excellent agreement with our 2012 prediction. This velocity corresponds to an approximate age of $t = 2672^{-817}_{+2102}$ yr. While consistent with the suggestion that the most recent nova eruption of Z Cam was the transient recorded by Chinese imperial astrologers in the year 77 bce, the age uncertainty is still too large to support or disprove a connection with Z Cam.

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Critical comments on publications by S. Hoffmann and N. Vogt on historical novae/supernovae and their candidates

Cited by 4 publications

References 49 publications

The Path from the Chinese and Japanese Observations of Supernova 1181 AD, to a Type Iax Supernova, to the Merger of CO and ONe White Dwarfs

The Path from the Chinese and Japanese Observations of Supernova 1181 AD, to a Type Iax Supernova, to the Merger of CO and ONe White Dwarfs

A list of guest‐star records in Korean history and their possible counterparts

Introducing the Condor Array Telescope – III. The expansion and age of the shell of the dwarf nova Z Camelopardalis, and detection of a second, larger shell

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