Sunspot characteristics of active regions NOAA 2268 and NOAA 2305

K. F. Lopez; V. S. Canedo; D. P. Cabezas; Y. J. Buleje

Sunspot characteristics of active regions NOAA 2268 and NOAA 2305

K. F. Lopez, V. S. Canedo, D. P. Cabezas, Y. J. Buleje

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution › peer-review

Abstract

In this paper we present a study of two solar active regions NOAA 2268 and NOAA 2305 observed on January 28 and 29, and also on March 24 and 25 of 2015, respectively. Such active regions produced multiple solar flares including M-class flares as classified in the soft X-ray scale using GOES observation. We mainly use sunspot sketches obtained with a 15 cm diameter Takahashi telescope located at Universidad Nacional San Luis Gonzaga de Ica, Peru. The active regions were characterized on the basis of the sunspots number and the magnetic configuration. We also derived the physical speed of the spots under study, resulting 1.69 and 1.76 km s - for the period of January and March, respectively. In addition, considering the calculated speeds we estimated the rotation period of the Sun for the dates mentioned above, which result in 28.9 days for January and 27.4 days for March. The present study is complemented with data taken by the Helioseismic and Magnetic Imager (HMI) instrument onboard the Solar Dynamics Observatory (SDO), which provides high resolution solar images in the continuum at 6173 Å as well as magnetograms.

Original language	Spanish
Title of host publication	Journal of Physics: Conference Series
Volume	1143
State	Published - 21 Dec 2018
Externally published	Yes

Cite this

@inproceedings{3070792559d84530983b94b4b96d13a7,

title = "Sunspot characteristics of active regions NOAA 2268 and NOAA 2305",

abstract = "In this paper we present a study of two solar active regions NOAA 2268 and NOAA 2305 observed on January 28 and 29, and also on March 24 and 25 of 2015, respectively. Such active regions produced multiple solar flares including M-class flares as classified in the soft X-ray scale using GOES observation. We mainly use sunspot sketches obtained with a 15 cm diameter Takahashi telescope located at Universidad Nacional San Luis Gonzaga de Ica, Peru. The active regions were characterized on the basis of the sunspots number and the magnetic configuration. We also derived the physical speed of the spots under study, resulting 1.69 and 1.76 km s - for the period of January and March, respectively. In addition, considering the calculated speeds we estimated the rotation period of the Sun for the dates mentioned above, which result in 28.9 days for January and 27.4 days for March. The present study is complemented with data taken by the Helioseismic and Magnetic Imager (HMI) instrument onboard the Solar Dynamics Observatory (SDO), which provides high resolution solar images in the continuum at 6173 {\AA} as well as magnetograms.",

author = "Lopez, {K. F.} and Canedo, {V. S.} and Cabezas, {D. P.} and Buleje, {Y. J.}",

year = "2018",

month = dec,

day = "21",

language = "Espa{\~n}ol",

volume = "1143",

booktitle = "Journal of Physics: Conference Series",

}

TY - GEN

T1 - Sunspot characteristics of active regions NOAA 2268 and NOAA 2305

AU - Lopez, K. F.

AU - Canedo, V. S.

AU - Cabezas, D. P.

AU - Buleje, Y. J.

PY - 2018/12/21

Y1 - 2018/12/21

N2 - In this paper we present a study of two solar active regions NOAA 2268 and NOAA 2305 observed on January 28 and 29, and also on March 24 and 25 of 2015, respectively. Such active regions produced multiple solar flares including M-class flares as classified in the soft X-ray scale using GOES observation. We mainly use sunspot sketches obtained with a 15 cm diameter Takahashi telescope located at Universidad Nacional San Luis Gonzaga de Ica, Peru. The active regions were characterized on the basis of the sunspots number and the magnetic configuration. We also derived the physical speed of the spots under study, resulting 1.69 and 1.76 km s - for the period of January and March, respectively. In addition, considering the calculated speeds we estimated the rotation period of the Sun for the dates mentioned above, which result in 28.9 days for January and 27.4 days for March. The present study is complemented with data taken by the Helioseismic and Magnetic Imager (HMI) instrument onboard the Solar Dynamics Observatory (SDO), which provides high resolution solar images in the continuum at 6173 Å as well as magnetograms.

AB - In this paper we present a study of two solar active regions NOAA 2268 and NOAA 2305 observed on January 28 and 29, and also on March 24 and 25 of 2015, respectively. Such active regions produced multiple solar flares including M-class flares as classified in the soft X-ray scale using GOES observation. We mainly use sunspot sketches obtained with a 15 cm diameter Takahashi telescope located at Universidad Nacional San Luis Gonzaga de Ica, Peru. The active regions were characterized on the basis of the sunspots number and the magnetic configuration. We also derived the physical speed of the spots under study, resulting 1.69 and 1.76 km s - for the period of January and March, respectively. In addition, considering the calculated speeds we estimated the rotation period of the Sun for the dates mentioned above, which result in 28.9 days for January and 27.4 days for March. The present study is complemented with data taken by the Helioseismic and Magnetic Imager (HMI) instrument onboard the Solar Dynamics Observatory (SDO), which provides high resolution solar images in the continuum at 6173 Å as well as magnetograms.

M3 - Contribución a la conferencia

VL - 1143

BT - Journal of Physics: Conference Series

ER -