Daniel Mögling’s Sunspot Observations in 1626–1629: A Manuscript Reference for the Solar Activity before the Maunder Minimum

Hayakawa, Hisashi; Iju, Tomoya; Murata, Koji; Besser, Bruno P.

doi:10.3847/1538-4357/abdd34

Cited by 14 publications

(9 citation statements)

References 42 publications

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“…In particular, the cross-calibration of records by individual observers has recently been debated (Clette & Lefèvre 2016Lockwood et al 2016;Usoskin et al 2016a). This led to the development of new techniques (Usoskin et al 2016b;Willamo et al 2017;Chatzistergos et al 2017), reanalysis of some data, and the recovery of additional sources (e.g., Arlt et al 2013Arlt et al , 2016Vaquero et al 2016;Carrasco et al 2018Carrasco et al , 2019Carrasco et al , 2021aHayakawa et al 2020aHayakawa et al ,b, 2021Vokhmyanin et al 2020), which improved the accuracy of the sunspot number records and thus irradiance reconstructions (Kopp et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Reconstructing solar irradiance from historical Ca II K observations

Chatzistergos

Krivova

Ermolli

et al. 2021

A&A

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Context. Knowledge of solar irradiance variability is critical to Earth’s climate models and understanding the solar influence on Earth’s climate. Direct solar irradiance measurements have only been available since 1978. Reconstructions of past variability typically rely on sunspot data. However, sunspot records provide only indirect information on the facular and network regions, which are decisive contributors to irradiance variability on timescales of the solar cycle and longer. Aims. Our ultimate goal is to reconstruct past solar irradiance variations using historical full-disc Ca II K observations to describe the facular contribution independently of sunspot observations. Here, we develop the method and test it extensively by using modern CCD-based (charge-coupled device) Ca II K observations. We also carry out initial tests on two photographic archives. Methods. We employ carefully reduced and calibrated Ca II K images from 13 datasets, including some of the most prominent series, such as those from the Meudon, Mt Wilson, and Rome observatories. We convert them to unsigned magnetic field maps and then use them as input to the adapted Spectral and Total Irradiance Reconstruction (SATIRE) model to reconstruct total solar irradiance (TSI) variations over the period 1978–2019, for which direct irradiance measurements are available. Results. The reconstructed irradiance from the analysed Ca II K archives agrees well with direct irradiance measurements and existing reconstructions. The model also returns good results on data taken with different bandpasses and images with low spatial resolution. Historical Ca II K archives suffer from numerous inconsistencies, but we show that these archives can still be used to reconstruct TSI with reasonable accuracy provided the observations are accurately processed and the effects of changes in instrumentation and instrumental parameters are identified and accounted for. The reconstructions are relatively insensitive to the TSI reference record used to fix the single free parameter of the model. Furthermore, even employment of a series, itself reconstructed from Ca II K data, as a reference for further reconstructions returns nearly equally accurate results. This will enable the Ca II K archives without an overlap with direct irradiance measurements to be used to reconstruct past irradiance. Conclusions. By using the unsigned magnetic maps of the Sun reconstructed from modern high-quality Ca II K observations as input into the SATIRE model, we can reconstruct solar irradiance variations nearly as accurately as from directly recorded magnetograms. Historical Ca II K observations can also be used for past irradiance reconstructions but need additional care, for example identifying and accounting for discontinuities and changes in the quality of the data with time.

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Section: Introductionmentioning

confidence: 99%

Reconstructing solar irradiance from historical Ca II K observations

Chatzistergos

Krivova

Ermolli

et al. 2021

A&A

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“…Only Scheiner recorded observations over more days in this interval (372 records). The other astronomers who made sunspot observations during this observation period were Malapert (17 records) and Hortensius (2 records) (V16; Hayakawa et al, 2021). Smogulecki was the only observer with records on 24 of his observation days.…”

Section: Sunspot Group Numbersmentioning

confidence: 94%

“…Carrasco et al (2021) have recently revised the sunspot observations recorded by Scheiner (1630Scheiner ( , 1651 in his books Rosa Ursina and Prodomus for the period 1611 -1632 correcting significant problems in the number of groups related to those observations in V16. Figure 3 (bottom panel) combines the new counting method developed in this work with those of Carrasco et al (2021) and Hayakawa et al (2021), in addition to the records included in V16 for the period 1610 -1632. The group counting obtained in this work from Smogulecki data is compatible with the values of the number of groups shown by Carrasco et al (2021) for the rising phase of the 1620s solar cycle.…”

Section: Sunspot Group Numbersmentioning

confidence: 99%

“…Carrasco et al (2019) also analysed the sunspot observations made by Malapert for the period 1618 -1626, obtaining a greater solar-activity level from these records than previously known. Hayakawa et al (2021) consulted the original manuscript of Mögling's sunspot observations and derived his sunspot-group number and sunspot positions for the period 1626 -1629. Arlt et al (2016) calculated the areas, latitudes, and tilt angles from sunspot drawings recorded by Scheiner in his book Rosa Ursina (Scheiner, 1630); further, Vokhmyanin and Zolotova (2018a,b) determined the group numbers, positions, and areas from Galileo's and Gassendi's observations.…”

Section: Introductionmentioning

confidence: 99%

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Analyses of Early Sunspot Records by Jean Tarde (1615 – 1617) and Jan Smogulecki (1621 – 1625)

et al. 2021

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Jean Tarde and Jan Smogulecki carried out sunspot observations in the 1610s and 1620s at the dawn of the telescopic era. We analysed their original observational records to revise their sunspot-group numbers in the existing database. In this study, we provide a new counting as a basis for future scientific discussions. Furthermore, we compared Smogulecki’s sunspot observations with those of Scheiner and Schönberger on the same observation days. We also detected a big sunspot group on 2 – 3 February 1622 in Smogulecki’s sunspot drawings and estimated its area to be approximately 1600 millionths of the solar disc. In addition, we measured the sunspot positions in Tarde’s and Smogulecki’s sunspot drawings to construct a butterfly diagram for this early period.

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“…In the last few years, the database of sunspot data has been scrutinised and updated to include more data (e.g. Vaquero et al 2016;Carrasco et al 2018Carrasco et al , 2020Carrasco et al , 2021Hayakawa et al 2020aHayakawa et al ,b, 2021Vokhmyanin et al 2020). Also, the method on how to include individual sunspot series has been a matter of debate (Lockwood et al 2016;Usoskin et al 2016a).…”

Section: Introductionmentioning

confidence: 99%

Scrutinising the relationship between plage areas and sunspot areas and numbers

Chatzistergos

Ermolli

Krivova

et al. 2022

A&A

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Context. Studies and reconstructions of past solar activity require data on all magnetic regions on the surface of the Sun (i.e. on dark sunspots as well as bright faculaeplage and network). Such data are also important for understanding the magnetic activity and variability of the Sun and Sun-like stars. The longest available direct faculaeplage datasets are white-light facular and Ca ii K observations going back to 1874 and 1892, respectively. Prior to that time the only direct data available are for sunspots. Aims. We reassess the relationship between plage areas and sunspot records (areas and numbers) since 1892, to allow reconstructions of facularplage areas which can be employed for studies going further back in time to the period when solely sunspot observations are available. Methods. We use the plage areas derived from 38 consistently processed Ca ii K archives as well as the plage area composite based on these archives. The considered archives include both the well-known observatories (e.g. Coimbra, Kodaikanal, Meudon, Mt Wilson), and the less explored observatories (e.g. Kharkiv, Mees, and Upice). These data allow us to study the relationship between plage area and sunspot records (areas and number) over a period of 12 solar cycles and for dierent bandpasses. Results. We nd the relationship between plage and sunspot areas to be well represented by a power-law function; the relationship between the plage areas and the sunspot number is also best t with a power-law function. We further nd that the relationships depend on the bandwidth and the solar cycle strength. The reconstructions with a power-law relationship are in good agreement with the original plage area series, whereas employment of a cycle-strength-dependent relationship improves the reconstructions only marginally. We also estimate the error in the plage areas reconstructed from the sunspot areas or numbers. Performing the same analysis on other previously published plage area series, usually derived from a single archive with diverse processing techniques, returns dierent results when using dierent time series. This highlights the importance of applying a consistent processing to the various archives and demonstrates the uncertainties introduced by using previously published series for studies of past solar activity, including irradiance reconstructions. Conclusions. Our results have implications for past solar activity and irradiance reconstructions and for stellar activity studies, which sometimes assume a linear dependence between plage and sunspot areas.

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Daniel Mögling’s Sunspot Observations in 1626–1629: A Manuscript Reference for the Solar Activity before the Maunder Minimum

Cited by 14 publications

References 42 publications

Reconstructing solar irradiance from historical Ca II K observations

Reconstructing solar irradiance from historical Ca II K observations

Analyses of Early Sunspot Records by Jean Tarde (1615 – 1617) and Jan Smogulecki (1621 – 1625)

Scrutinising the relationship between plage areas and sunspot areas and numbers

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