Das Verhalten von T Coronae Borealis in neuerer Zeit

Ferrari, Kevin

doi:10.1002/asna.19352561705

Cited by 2 publications

(1 citation statement)

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“…The plate collection at Bamberg Observatory, in Germany, has a good collection of plates that covers the 1930s. Bohme (1938) and Ferrari (1935) have already published 139 𝐵 magnitudes for T CrB, although I have had to convert their old magnitudes to modern 𝐵 magnitudes by detailed analysis of their stated comparison stars and their adopted sequences of magnitudes. Further, I have found one previously-unused box of plates in the Bamberg archives, and this provides 16 more 𝐵 magnitudes from 1932-1939.…”

Section: Photographic Magnitudesmentioning

confidence: 99%

The B & V Light Curves for Recurrent Nova T CrB From 1842--2022, the Unique Pre- and Post-Eruption High-States, the Complex Period Changes, and the Upcoming Eruption in 2025.5$\pm$1.3

Schaefer¹

2023

Preprint

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T CrB is one of the most-famous and brightest novae known, and is a recurrent nova with prior eruptions in 1866 and 1946 that peak at 𝑉=2.0. I have constructed light curves spanning 1842-2022 with 213,730 magnitudes, where the 𝐵 and 𝑉 magnitudes are fully corrected to the Johnson system. These light curves first reveal a unique complex high-state (with 20× higher accretion rate than the normal low-state) stretching from -10 to +9 years after eruption, punctuated with a deep pre-eruption dip (apparently from dust formation in a slow mass ejection) and a unique enigmatic secondary eruption (with 10 per cent of the energy of the primary eruption), with the light curves identical for the 1866 and 1946 eruptions. Starting in 2015, T CrB entered the high-state, like in 1936, so a third eruption in upcoming years has been widely anticipated. With the pre-1946 light curve as a template, I predict a date of 2025.5±1.3 for the upcoming eruption, with the primary uncertainty arising from a possible lengthening of the pre-eruption high-state. I use the large-amplitude ellipsoidal modulation to track the orbital phase of the binary from 1867-2022. I measure that the orbital period increased abruptly by +0.185±0.056 days across the 1946 eruption, the 1947-2022 years had a steady period decrease of (−8.9±1.6)×10 −6 days-per-day, and the 1867-1946 years had a steady period change consistent with zero, at (+1.75±4.5)×10 −6 days-per-day. These large period changes cannot be explained by any published mechanism.

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Section: Photographic Magnitudesmentioning

confidence: 99%

The B & V Light Curves for Recurrent Nova T CrB From 1842--2022, the Unique Pre- and Post-Eruption High-States, the Complex Period Changes, and the Upcoming Eruption in 2025.5$\pm$1.3

Schaefer¹

2023

Preprint

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The B & V light curves for recurrent nova T CrB from 1842–2022, the unique pre- and post-eruption high-states, the complex period changes, and the upcoming eruption in 2025.5 ± 1.3

Schaefer

2023

Monthly Notices of the Royal Astronomical Society

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T CrB is one of the most-famous and brightest novae known, and is a recurrent nova with prior eruptions in 1866 and 1946 that peak at V = 2.0. I have constructed light curves spanning 1842–2022 with 213,730 magnitudes, where the B and V magnitudes are fully corrected to the Johnson system. These light curves first reveal a unique complex high-state (with 20× higher accretion rate than the normal low-state) stretching from -10 to +9 years after eruption, punctuated with a deep pre-eruption dip (apparently from dust formation in a slow mass ejection) and a unique enigmatic secondary eruption (with 10 per cent of the energy of the primary eruption), with the light curves identical for the 1866 and 1946 eruptions. Starting in 2015, T CrB entered the high-state, like in 1936, so a third eruption in upcoming years has been widely anticipated. With the pre-1946 light curve as a template, I predict a date of 2025.5 ± 1.3 for the upcoming eruption, with the primary uncertainty arising from a possible lengthening of the pre-eruption high-state. I use the large-amplitude ellipsoidal modulation to track the orbital phase of the binary from 1867–2022. I measure that the orbital period increased abruptly by +0.185 ± 0.056 days across the 1946 eruption, the 1947–2022 years had a steady period decrease of (−8.9 ± 1.6) × 10−6 days-per-day, and the 1867–1946 years had a steady period change consistent with zero, at (+1.75 ± 4.5) × 10−6 days-per-day. These large period changes cannot be explained by any published mechanism.

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Das Verhalten von T Coronae Borealis in neuerer Zeit

Cited by 2 publications

References 0 publications

The B & V Light Curves for Recurrent Nova T CrB From 1842--2022, the Unique Pre- and Post-Eruption High-States, the Complex Period Changes, and the Upcoming Eruption in 2025.5$\pm$1.3

The B & V Light Curves for Recurrent Nova T CrB From 1842--2022, the Unique Pre- and Post-Eruption High-States, the Complex Period Changes, and the Upcoming Eruption in 2025.5$\pm$1.3

The B & V light curves for recurrent nova T CrB from 1842–2022, the unique pre- and post-eruption high-states, the complex period changes, and the upcoming eruption in 2025.5 ± 1.3

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