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7 results for “Sunspots”
Kodaikanal Solar Observatory (KoSO) White-Light Sunspot Regions Masks (1904-2017)
<p>Regular observations at the Kodaikanal Solar Observatory (KoSO) began in 1904 using a white-light telescope with a 10-cm aperture lens and an f/15 light beam. Between 1912 and 1917, the objective lens was changed several times. In 1918, a 15-cm achromatic lens was installed. This new configuration produced a 20.4 cm size image of the Sun in the image plane. Photographic plates were used to capture the image. The same telescope has been used since 1918 up until 2017 to take regular white-light observations of the Sun. This data set provides the sunspot mask in HDF5 format for all the White Light Observations acquired at KoSO. Each HDF5 file contains the sunspot mask for all the observations for that year. The sunspot masks are provided in two different coordinate systems: (i) Full Disk as observed and (ii) Carrington heliographic coordinate, which is transformed from full disk using near point interpolation. Each data set also contains metadata in the form of HDF5 attributes. The Carrington co-ordinate data if full Sun map, hence the near-side of the Sun is the region where values in the mask in non-zero, where as sunspot regions are filled with value 2. </p> <p>A <strong>Python package (KoSOpy), which can be located on <a href="https://github.com/Kodaikanal-Solar-Observatory/kosopy" target="_blank" rel="noopener">GitHub</a>,</strong> is being developed which can be used to navigate through these data sets.</p>
Sunspot Group Database of the Specola Solare Ticinese
<p><strong>Content:</strong></p> <p>The database contains data for each sunspot group observed and recorded at the Specola Solare Ticinese from 01.06.1957 until 31.12.2024. Recorded for each group are the date and time of observation, code for the observer, the sky quality during observation, the incremental number, the weighted count, the unweighted count (if available), the Zurich classification, the latitude and longitude determined with Digisun (a free software developed by SILSO for measuring and recording sunspot groups features) or, if these are not available, the latitude and longitude determined manually with the Stonyhurst solar disk, the ETHZ signature, and the DOI code of the drawing. </p> <p> </p> <p><strong>Context:</strong></p> <p>The daily sunspot drawings are performed at Specola Solare Ticinese since 1957. Between 1957 and 1980 Specola was the southern observing station belonging to the Eidgenössische Sternwarte of ETH Zurich (director prof. Max Waldmeier). Since 1981 Specola is operated independently by the local Associazione Specola Solare Ticinese. The corresponding sunspot drawings up to 2019 are archived at the ETH-Zurich University Archives with codes HS1304.5 (1957-1980) and HS1304.6 (1981-2019). They are also available in digital format on the platform e-manuscripta ( https://www.e-manuscripta.ch/). The sunspot drawings made after 2020 are archived at Specola Solare Ticinese and the digital version is made available on the site https://sunspots.irsol.usi.ch/.</p> <p>The main purpose of the drawings is to determine the relative number (R) of the solar activity (called also <em>Wolf number </em>or <em>Sunspot Number</em>). In this context the Specola is considered as the pilot station by the world data center SILSO (Sunspot Index and Long-term Solar Observations) in Bruxelles, whose main goal is the production, preservation and dissemination of the international sunspot number. The relative number is calculated according to the formula R = k.(10.g+f) introduced by Rudolf Wolf, where g is the number of sunspot groups, f the number of sunspots and k is a reduction factor which depends from the observer, the instrument and the observing conditions. </p> <p> </p> <p>The drawings are always performed with the white light projection method (diameter of the Sun image 250 mm) according to the Zurich standard. A Zeiss Coudé refractor is used (D/f 150/2250 mm baffled at 8 cm). The drawings are oriented with a precision of ±1° with respect to the heliographic axis. When the seeing is good enough (most of the cases), the quality of the sunspot drawings details is accurate and can be used for the morphological analysis of sunspot groups and for the determination of their heliographic position. </p> <p> </p> <p>The obtained image is specular: heliographic North above and eastern limb on the right. </p> <p> </p> <p>For more information: </p> <p>https://www.specola.ch/en/sunspot-drawings-of-the-specola-solare-ticinese/sunspot-drawings-of-the-specola-solare-ticinese</p> <p>All observations can be found here:</p> <p>https://sunspots.irsol.usi.ch/</p> <p> </p> <p><strong>Columns explanation:</strong> </p> <p> </p> <ul> <li>date </li> </ul> <p>Observation date </p> <p> </p> <ul> <li>time </li> </ul> <p>Observation time (UT) </p> <p> </p> <ul> <li>observer </li> </ul> <p>Observer identifier, according to following list </p> <p> </p> <p>Sergio Cortesi: 1 </p> <p>Edy Alge: 2 </p> <p>Elena Altoni: 3 </p> <p>Michele Bianda: 4 </p> <p>Araldo Pittini: 5 </p> <p>Andrea Manna: 6 </p> <p>Renzo Ramelli: 7 </p> <p>Marco Cagnotti: 8 </p> <p>Anna Cairati: 9 </p> <p>Roberto Cortesi: 10 </p> <p>Michele DeLorenzi: 11 </p> <p>Marco Cortesi: 12 </p> <p>J. Jzsák: 13 </p> <p>Rolf Schmid: 14 </p> <p> </p> <ul> <li>seeing (SIDC) </li> </ul> <p>Quality of the sky during the observation (5=best, 1=very bad) </p> <p> </p> <ul> <li>group nr </li> </ul> <p>Incremental sunspot group number (starting from the beginning of the year) </p> <p> </p> <ul> <li>spot count </li> </ul> <p>Unweighed sunspot counting </p> <p> </p> <ul> <li>weighted spot count </li> </ul> <p>Weighted sunspot counting following the Waldmeier's rule </p> <p>Cortesi, S., Cagnotti, M., Bianda, M. et al. Sunspot Observations and Counting at Specola Solare Ticinese in Locarno Since 1957. Sol Phys 291, 3075–3080 (2016). https://doi.org/10.1007/s11207-016-0872-7 </p> <p>https://link.springer.com/article/10.1007/s11207-016-0872-7 </p> <p> </p> <ul> <li>type </li> </ul> <p>Zurich classification of the sunspots group </p> <p> </p> <ul> <li>latitude </li> </ul> <p>Heliographic group floating point precision latitude (±1°) determined with DigiSun software </p> <p> </p> <ul> <li>longitude </li> </ul> <p>Heliographic group floating point longitude (±1°) determined with DigiSun software </p> <p> </p> <ul> <li>manual latitude </li> </ul> <p>Heliographic group integer latitude (±1°) detetermined manually with Stonyhurst solar disk </p> <p> </p> <ul> <li>manual longitude </li> </ul> <p>Heliographic group integer longitude (±1°) with Stonyhurst solar disk </p> <p> </p> <ul> <li>ETHZ signature </li> </ul> <p>Drawing-specific signature of the ETH Zurich University Archive </p> <p> </p> <ul> <li>URL</li> </ul> <p>URL of the digitized sunspot drawing file. </p> <p> </p> <p> </p>
Dataset for "The Dependence of Solar Flare Magnitude on Sunspot Area During Activity Cycle 24"
<p>Dataset for of Will, Avallone, & Sun (2022), RNAAS, 6, 37 "The Dependence of Solar Flare Magnitude on Sunspot Area During Activity Cycle 24". </p> <p>This is a .cvs file containing the information of 412 solar active regions, including their NOAA numbers, sunspot area, sunspot classification, and the peak GOES soft X-ray flux of the largest flare it produced. The sunspot area data are measured using continuum images from SDO/HMI.</p>
Daily solar data and sunspot region summary of 23-24 solar cycle
<p>This dataset contains records of daily solar data as well as data collected from magnetic classes...</p> <p>This dataset was assembled with data from ftp://ftp.swpc.noaa.gov/pub/warehouse/.</p> <p>The date the data was assembled is 2017-01-15 (yyyy-mm-dd).</p> <p>The original data source is provided by the Space Weather Prediction Center - SWPC, which is linked to the National Oceanic and Atmospheric Administration - NOAA from US Department of Commerce.</p> <p>Data description:</p> <ul> <li><strong>radio_flux_10.7cm</strong>: the solar radio flux at 10.7 cm (2800 MHz) is an indicator of solar activity. It is also called the F10.7 index and is one of the longest running records of solar activity. Radio emissions originate high in the chromosphere and low in the corona of the solar atmosphere.</li> <li><strong>sesc_sunspot_number</strong>: it refers to the number of sunspots computed on a given day. Also called Wolf's number of sunspots, it is given by R = k(10g + s), where k is a scalable factor indicating the combined effects of observation conditions, g is the number of active regions and s the number of sunspots in all these groups.</li> <li><strong>sunspot_area</strong>: it refers to the sum of the corrected area of all observed sunspots. It is measured in units of millionths of the solar hemisphere.</li> <li><strong>goes15_xray_bkgd_flux</strong>: it corresponds to the daily average background X-ray flux that is measured by the SWPC primary GOES satellite. To calculate this value, sensors register 24 X-ray measures for a given day, one for each hour. Then, the SWPC creates 3 groups of periods of 8 hours. For these groups, the SWPC registers the lowest values of flux, creating 3 minimal values, one for each group. Then, they calculate the average between the minimum values of the first and the third group. After the average calculation, they must compare this value to the minimal value of the second group. The minimum value from the last comparison gives the result of the X-ray background flux.</li> <li><strong>mwl_alpha</strong>: binary attribute indicating the presence of apha magnetic class in any observed spot.</li> <li><strong>mwl_beta</strong>: binary attribute indicating the presence of beta magnetic class in any observed spot.</li> <li><strong>mwl_gamma</strong>: binary attribute indicating the presence of gamma magnetic class in any observed spot.</li> <li><strong>mwl_beta_gamma</strong>: binary attribute indicating the presence of beta-gamma magnetic class in any observed spot.</li> <li><strong>mwl_delta</strong>: binary attribute indicating the presence of delta magnetic class in any observed spot.</li> <li><strong>mwl_beta_delta</strong>: binary attribute indicating the presence of beta-delta magnetic class in any observed spot.</li> <li><strong>mwl_beta_gamma_delta</strong>: binary attribute indicating the presence of beta-gamma-delta magnetic class in any observed spot.</li> <li><strong>mwl_gamma_delta</strong>: binary attribute indicating the presence of gamma-delta magnetic class in any observed spot.</li> <li><strong>c_class_flares</strong>: number of c class flares observed.</li> <li><strong>m_class_flares</strong>: number of m class flares observed.</li> <li><strong>x_class_flares</strong>: number of x class flares observed.</li> </ul> <p>The data collected refer to the period between january 01, 1997 to january 15, 2017.</p> <p> </p>
Magnetic field line information from sunspot simulation in 10.5281/zenodo.6385593
<p>This dataset contains magnetic field line information from the dataset corresponding to 10.5281/zenodo.6385593</p>
Variables from several snapshots of 0% net helicity driven sunspot simulation
<p>The included dataset is from an magnetohydrodynamic simulation of a sunspot that is driven by photospheric motions. Several snapshots in time are extracted, and the magnetic field, velocity, and current from those snapshots is stored in the attached dataset, along with the three coordinate arrays. The datafiles are in HDF5 format, which is easily read in all major programming languages. The simulation is largely described in https://ui.adsabs.harvard.edu/abs/2017ApJ...851L..17K/abstract. The files are read directly from the restart files and the variables reside at their original grid locations. The files labeled fieldline.* are fortran unformatted datasets of magnetic field lines traced from the boundary of the simulation at these time steps. The dimensions of the traced field lines are 401x401x400x3.</p>
Clinical Study to Assess Safety, Efficacy and In-Use Tolerability of Oziva Bioactive Gluta Fizzy Effervescent Tablets on Subjects With Facial Dark Spots Such as Pimple Marks, Sunspots, Age Spots and U
ClinicalTrials.gov study NCT07162623. IPD Sharing: NO. Countries: 1. Publications: 0.
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