1:45 PM - 3:15 PM
[O11-P64] The photometry of W UMa, variable star, with Seestar
Keywords:Seestar S50, Variable star, W UMa
Purpose
Recently, equipment such as Seestar, which can automatically introduce celestial objects and take pictures of them by operating an app, has appeared.
In the case of Seestar, primary processing (darkening, etc.) of astronomical images is also done automatically.
primary processing (darkening, etc.) of astro-images is also done automatically, making astrophotography and image processing easier and more comfortable.
and image processing is easier and more comfortable. We investigated whether Seestar can be used to observe changes in the magnitude of variable stars.
Seestar is an instrument that is used to observe the magnitude changes of variable stars.
What is Seestar?
Seestar is a telescope for telescopic observation, and its small size and light weight make it easy to set up and take down, and it can be used for immediate observation without worrying about its orientation.
It can be set up and taken down easily because of its small size and light weight, and can be used for immediate observation without worrying about its azimuth.
Research Method
In this study, Seestar is used in place of a single-lens reflex camera or a cooled CCD camera.
Since Seestar saves the captured data as a fits file, it is possible to obtain the count value using Makali without changing the saved file.
The data is saved as a fits file, so the count values are obtained by Macari, and the grade is determined. The procedure is as follows: I. Using Seestar
Observe and photograph W UMa and the reference star. This time, observations were made from the night of November 25, 2024 to the dawn of November 26, 2024.
The observation was made from the night of November 25 to the dawn of November 26, 2024. Exposure time was 10 seconds and stacking was at least 10 images.
The count values of W UMa and the reference star were obtained using Makali.
Read the fits file into Makali and perform photometry of W UMa and the reference star using “Aperture Photometry”. All count values are available in the photometry results window.
The fits file that meets the conditions is all in this file. Do this for all fits files that meet the requirements.
The magnitude of W UMa is obtained from the count values using Excel, and the change in magnitude with time is plotted on a graph. (W
UMa count value) = la (count value of the reference star) = lb (magnitude of the reference star) = mb, then (W UMa's
magnitude) = mb - 5 / 2 log 10 (la / lb) This formula was used to obtain the magnitude of W UMa.
What is W UMa?
W UMa is a dwarf eclipsing binary system in the direction of Ursa Major, in which two F-type main-sequence stars are in contact and share an atmosphere.
The orbital period is about 8 hours. The orbital period is about 8 hours, during which the eclipses occur twice. Since the two stars are almost
The depths of the two eclipses are similar because the stars are almost the same. The visual magnitudes are 7.75-8.48.
Results
The result of obtaining the magnitude using the reference star with the smallest magnitude difference range is shown in the attached figure.
Discussion
The figure shows that there were three changes in magnitude during the 12-hour period from 19:00 to 7:00. The difference was about 0.7 mag.
The difference was about 0.7 mag, which is consistent with the magnitude difference already known. The magnitude difference was in agreement with the eclipsing
The minimum time of this figure is almost the same as that of the eclipsing variable predicted by Kazuo Nagai. This indicates that SeeStar can be used as a
We believe that SeeStar is a useful instrument to use in the study of eclipsing variable stars.
Future Prospects
We were able to follow the changes in magnitude of short-period variable stars such as W UMa in this observation.
We would like to confirm if it is possible to make similar observations of long-period variable stars and novas.
We would like to confirm whether we can make similar observations of long-period variable stars and novas. We would also like to try to estimate physical quantities such as mass
I would also like to try to estimate physical quantities such as masses obtained from changes in period and magnitude.
Recently, equipment such as Seestar, which can automatically introduce celestial objects and take pictures of them by operating an app, has appeared.
In the case of Seestar, primary processing (darkening, etc.) of astronomical images is also done automatically.
primary processing (darkening, etc.) of astro-images is also done automatically, making astrophotography and image processing easier and more comfortable.
and image processing is easier and more comfortable. We investigated whether Seestar can be used to observe changes in the magnitude of variable stars.
Seestar is an instrument that is used to observe the magnitude changes of variable stars.
What is Seestar?
Seestar is a telescope for telescopic observation, and its small size and light weight make it easy to set up and take down, and it can be used for immediate observation without worrying about its orientation.
It can be set up and taken down easily because of its small size and light weight, and can be used for immediate observation without worrying about its azimuth.
Research Method
In this study, Seestar is used in place of a single-lens reflex camera or a cooled CCD camera.
Since Seestar saves the captured data as a fits file, it is possible to obtain the count value using Makali without changing the saved file.
The data is saved as a fits file, so the count values are obtained by Macari, and the grade is determined. The procedure is as follows: I. Using Seestar
Observe and photograph W UMa and the reference star. This time, observations were made from the night of November 25, 2024 to the dawn of November 26, 2024.
The observation was made from the night of November 25 to the dawn of November 26, 2024. Exposure time was 10 seconds and stacking was at least 10 images.
The count values of W UMa and the reference star were obtained using Makali.
Read the fits file into Makali and perform photometry of W UMa and the reference star using “Aperture Photometry”. All count values are available in the photometry results window.
The fits file that meets the conditions is all in this file. Do this for all fits files that meet the requirements.
The magnitude of W UMa is obtained from the count values using Excel, and the change in magnitude with time is plotted on a graph. (W
UMa count value) = la (count value of the reference star) = lb (magnitude of the reference star) = mb, then (W UMa's
magnitude) = mb - 5 / 2 log 10 (la / lb) This formula was used to obtain the magnitude of W UMa.
What is W UMa?
W UMa is a dwarf eclipsing binary system in the direction of Ursa Major, in which two F-type main-sequence stars are in contact and share an atmosphere.
The orbital period is about 8 hours. The orbital period is about 8 hours, during which the eclipses occur twice. Since the two stars are almost
The depths of the two eclipses are similar because the stars are almost the same. The visual magnitudes are 7.75-8.48.
Results
The result of obtaining the magnitude using the reference star with the smallest magnitude difference range is shown in the attached figure.
Discussion
The figure shows that there were three changes in magnitude during the 12-hour period from 19:00 to 7:00. The difference was about 0.7 mag.
The difference was about 0.7 mag, which is consistent with the magnitude difference already known. The magnitude difference was in agreement with the eclipsing
The minimum time of this figure is almost the same as that of the eclipsing variable predicted by Kazuo Nagai. This indicates that SeeStar can be used as a
We believe that SeeStar is a useful instrument to use in the study of eclipsing variable stars.
Future Prospects
We were able to follow the changes in magnitude of short-period variable stars such as W UMa in this observation.
We would like to confirm if it is possible to make similar observations of long-period variable stars and novas.
We would like to confirm whether we can make similar observations of long-period variable stars and novas. We would also like to try to estimate physical quantities such as mass
I would also like to try to estimate physical quantities such as masses obtained from changes in period and magnitude.