Intensity contrast of solar network and faculae close to the solar limb, observed from two vantage points

Intensity contrast of solar network and faculae close to the solar limb, observed from two vantage points

Context. The brightness of faculae and network depends on the angle at which they are observed and the magnetic flux density. Close to the limb, the assessment of this relationship has until now been hindered by the increasingly lower signal in magnetograms. Aims. This preliminary study aims to high...

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Veröffentlicht in:Astronomy and astrophysics (Berlin) 2023-10, Vol.678, p.A163
Hauptverfasser: Albert, K., Krivova, N. A., Hirzberger, J., Solanki, S. K., Moreno Vacas, A., Orozco Suárez, D., Albelo Jorge, N., Appourchaux, T., Alvarez-Herrero, A., Blanco Rodríguez, J., Gandorfer, A., Gutierrez-Marques, P., Kahil, F., Kolleck, M., Volkmer, R., del Toro Iniesta, J. C., Woch, J., Fiethe, B., Pérez-Grande, I., Sanchis Kilders, E., Balaguer Jiménez, M., Bellot Rubio, L. R., Calchetti, D., Carmona, M., Deutsch, W., Feller, A., Fernandez-Rico, G., Fernández-Medina, A., García Parejo, P., Gasent Blesa, J. L., Gizon, L., Grauf, B., Heerlein, K., Korpi-Lagg, A., Lange, T., López Jiménez, A., Maue, T., Meller, R., Müller, R., Nakai, E., Schmidt, W., Schou, J., Sinjan, J., Staub, J., Strecker, H., Torralbo, I., Valori, G.
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container_title Astronomy and astrophysics (Berlin)
container_volume 678
creator Albert, K.
Krivova, N. A.
Hirzberger, J.
Solanki, S. K.
Moreno Vacas, A.
Orozco Suárez, D.
Albelo Jorge, N.
Appourchaux, T.
Alvarez-Herrero, A.
Blanco Rodríguez, J.
Gandorfer, A.
Gutierrez-Marques, P.
Kahil, F.
Kolleck, M.
Volkmer, R.
del Toro Iniesta, J. C.
Woch, J.
Fiethe, B.
Pérez-Grande, I.
Sanchis Kilders, E.
Balaguer Jiménez, M.
Bellot Rubio, L. R.
Calchetti, D.
Carmona, M.
Deutsch, W.
Feller, A.
Fernandez-Rico, G.
Fernández-Medina, A.
García Parejo, P.
Gasent Blesa, J. L.
Gizon, L.
Grauf, B.
Heerlein, K.
Korpi-Lagg, A.
Lange, T.
López Jiménez, A.
Maue, T.
Meller, R.
Müller, R.
Nakai, E.
Schmidt, W.
Schou, J.
Sinjan, J.
Staub, J.
Strecker, H.
Torralbo, I.
Valori, G.
description Context. The brightness of faculae and network depends on the angle at which they are observed and the magnetic flux density. Close to the limb, the assessment of this relationship has until now been hindered by the increasingly lower signal in magnetograms. Aims. This preliminary study aims to highlight the potential of using simultaneous observations from different vantage points to better determine the properties of faculae close to the limb. Methods. We used data from the Solar Orbiter/Polarimetric and Helioseismic Imager (SO/PHI), and the Solar Dynamics Observatory/Helioseismic and Magnetic Imager (SDO/HMI), recorded at an ∼60° angular separation of their lines of sight at the Sun. We used the continuum intensity observed close to the limb by SO/PHI and complemented it with the co-observed B LOS from SDO/HMI, originating closer to disc centre (as seen by SDO/HMI), thus avoiding the degradation of the magnetic field signal near the limb. Results. We derived the dependence of facular brightness in the continuum on disc position and magnetic flux density from the combined observations of SO/PHI and SDO/HMI. Compared with a single point of view, we were able to obtain contrast values reaching closer to the limb and to lower field strengths. We find the general dependence of the limb distance at which the contrast is maximum on the flux density to be at large in line with single viewpoint observations, in that the higher the flux density is, the closer the turning point lies to the limb. There is a tendency, however, for the maximum to be reached closer to the limb when determined from two vantage points. We note that due to the preliminary nature of this study, these results must be taken with caution. Conclusions. Our analysis shows that studies involving two viewpoints can significantly improve the detection of faculae near the solar limb and the determination of their brightness contrast relative to the quiet Sun.
doi_str_mv 10.1051/0004-6361/202346037
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A. ; Hirzberger, J. ; Solanki, S. K. ; Moreno Vacas, A. ; Orozco Suárez, D. ; Albelo Jorge, N. ; Appourchaux, T. ; Alvarez-Herrero, A. ; Blanco Rodríguez, J. ; Gandorfer, A. ; Gutierrez-Marques, P. ; Kahil, F. ; Kolleck, M. ; Volkmer, R. ; del Toro Iniesta, J. C. ; Woch, J. ; Fiethe, B. ; Pérez-Grande, I. ; Sanchis Kilders, E. ; Balaguer Jiménez, M. ; Bellot Rubio, L. R. ; Calchetti, D. ; Carmona, M. ; Deutsch, W. ; Feller, A. ; Fernandez-Rico, G. ; Fernández-Medina, A. ; García Parejo, P. ; Gasent Blesa, J. L. ; Gizon, L. ; Grauf, B. ; Heerlein, K. ; Korpi-Lagg, A. ; Lange, T. ; López Jiménez, A. ; Maue, T. ; Meller, R. ; Müller, R. ; Nakai, E. ; Schmidt, W. ; Schou, J. ; Sinjan, J. ; Staub, J. ; Strecker, H. ; Torralbo, I. ; Valori, G.</creator><creatorcontrib>Albert, K. ; Krivova, N. A. ; Hirzberger, J. ; Solanki, S. 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Close to the limb, the assessment of this relationship has until now been hindered by the increasingly lower signal in magnetograms. Aims. This preliminary study aims to highlight the potential of using simultaneous observations from different vantage points to better determine the properties of faculae close to the limb. Methods. We used data from the Solar Orbiter/Polarimetric and Helioseismic Imager (SO/PHI), and the Solar Dynamics Observatory/Helioseismic and Magnetic Imager (SDO/HMI), recorded at an ∼60° angular separation of their lines of sight at the Sun. We used the continuum intensity observed close to the limb by SO/PHI and complemented it with the co-observed B LOS from SDO/HMI, originating closer to disc centre (as seen by SDO/HMI), thus avoiding the degradation of the magnetic field signal near the limb. Results. We derived the dependence of facular brightness in the continuum on disc position and magnetic flux density from the combined observations of SO/PHI and SDO/HMI. Compared with a single point of view, we were able to obtain contrast values reaching closer to the limb and to lower field strengths. We find the general dependence of the limb distance at which the contrast is maximum on the flux density to be at large in line with single viewpoint observations, in that the higher the flux density is, the closer the turning point lies to the limb. There is a tendency, however, for the maximum to be reached closer to the limb when determined from two vantage points. We note that due to the preliminary nature of this study, these results must be taken with caution. Conclusions. Our analysis shows that studies involving two viewpoints can significantly improve the detection of faculae near the solar limb and the determination of their brightness contrast relative to the quiet Sun.</description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 1432-0746</identifier><identifier>DOI: 10.1051/0004-6361/202346037</identifier><language>eng</language><ispartof>Astronomy and astrophysics (Berlin), 2023-10, Vol.678, p.A163</ispartof><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c294t-b2afee1adbf8fd071f1343f16ebd1b8fcf7a19e7082adca043844f7a87793093</citedby><cites>FETCH-LOGICAL-c294t-b2afee1adbf8fd071f1343f16ebd1b8fcf7a19e7082adca043844f7a87793093</cites><orcidid>0000-0001-8829-1938 ; 0000-0002-2391-6156 ; 0000-0001-9358-5834 ; 0000-0002-3418-8449 ; 0000-0002-7336-0926 ; 0000-0002-5387-636X ; 0000-0002-1377-3067 ; 0000-0002-3387-026X ; 0000-0002-1225-4177 ; 0000-0002-3776-9548 ; 0000-0001-9228-3412 ; 0000-0002-4792-1144 ; 0000-0002-9972-9840 ; 0000-0003-1459-7074 ; 0000-0003-1483-4535 ; 0000-0001-7696-8665 ; 0000-0002-1232-4315 ; 0000-0002-7145-2835 ; 0000-0003-2755-5295 ; 0000-0001-7809-0067 ; 0000-0001-9272-6439 ; 0000-0001-8669-8857</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,776,780,3714,27901,27902</link.rule.ids></links><search><creatorcontrib>Albert, K.</creatorcontrib><creatorcontrib>Krivova, N. A.</creatorcontrib><creatorcontrib>Hirzberger, J.</creatorcontrib><creatorcontrib>Solanki, S. K.</creatorcontrib><creatorcontrib>Moreno Vacas, A.</creatorcontrib><creatorcontrib>Orozco Suárez, D.</creatorcontrib><creatorcontrib>Albelo Jorge, N.</creatorcontrib><creatorcontrib>Appourchaux, T.</creatorcontrib><creatorcontrib>Alvarez-Herrero, A.</creatorcontrib><creatorcontrib>Blanco Rodríguez, J.</creatorcontrib><creatorcontrib>Gandorfer, A.</creatorcontrib><creatorcontrib>Gutierrez-Marques, P.</creatorcontrib><creatorcontrib>Kahil, F.</creatorcontrib><creatorcontrib>Kolleck, M.</creatorcontrib><creatorcontrib>Volkmer, R.</creatorcontrib><creatorcontrib>del Toro Iniesta, J. C.</creatorcontrib><creatorcontrib>Woch, J.</creatorcontrib><creatorcontrib>Fiethe, B.</creatorcontrib><creatorcontrib>Pérez-Grande, I.</creatorcontrib><creatorcontrib>Sanchis Kilders, E.</creatorcontrib><creatorcontrib>Balaguer Jiménez, M.</creatorcontrib><creatorcontrib>Bellot Rubio, L. R.</creatorcontrib><creatorcontrib>Calchetti, D.</creatorcontrib><creatorcontrib>Carmona, M.</creatorcontrib><creatorcontrib>Deutsch, W.</creatorcontrib><creatorcontrib>Feller, A.</creatorcontrib><creatorcontrib>Fernandez-Rico, G.</creatorcontrib><creatorcontrib>Fernández-Medina, A.</creatorcontrib><creatorcontrib>García Parejo, P.</creatorcontrib><creatorcontrib>Gasent Blesa, J. L.</creatorcontrib><creatorcontrib>Gizon, L.</creatorcontrib><creatorcontrib>Grauf, B.</creatorcontrib><creatorcontrib>Heerlein, K.</creatorcontrib><creatorcontrib>Korpi-Lagg, A.</creatorcontrib><creatorcontrib>Lange, T.</creatorcontrib><creatorcontrib>López Jiménez, A.</creatorcontrib><creatorcontrib>Maue, T.</creatorcontrib><creatorcontrib>Meller, R.</creatorcontrib><creatorcontrib>Müller, R.</creatorcontrib><creatorcontrib>Nakai, E.</creatorcontrib><creatorcontrib>Schmidt, W.</creatorcontrib><creatorcontrib>Schou, J.</creatorcontrib><creatorcontrib>Sinjan, J.</creatorcontrib><creatorcontrib>Staub, J.</creatorcontrib><creatorcontrib>Strecker, H.</creatorcontrib><creatorcontrib>Torralbo, I.</creatorcontrib><creatorcontrib>Valori, G.</creatorcontrib><title>Intensity contrast of solar network and faculae close to the solar limb, observed from two vantage points</title><title>Astronomy and astrophysics (Berlin)</title><description>Context. The brightness of faculae and network depends on the angle at which they are observed and the magnetic flux density. Close to the limb, the assessment of this relationship has until now been hindered by the increasingly lower signal in magnetograms. Aims. This preliminary study aims to highlight the potential of using simultaneous observations from different vantage points to better determine the properties of faculae close to the limb. Methods. We used data from the Solar Orbiter/Polarimetric and Helioseismic Imager (SO/PHI), and the Solar Dynamics Observatory/Helioseismic and Magnetic Imager (SDO/HMI), recorded at an ∼60° angular separation of their lines of sight at the Sun. We used the continuum intensity observed close to the limb by SO/PHI and complemented it with the co-observed B LOS from SDO/HMI, originating closer to disc centre (as seen by SDO/HMI), thus avoiding the degradation of the magnetic field signal near the limb. Results. We derived the dependence of facular brightness in the continuum on disc position and magnetic flux density from the combined observations of SO/PHI and SDO/HMI. Compared with a single point of view, we were able to obtain contrast values reaching closer to the limb and to lower field strengths. We find the general dependence of the limb distance at which the contrast is maximum on the flux density to be at large in line with single viewpoint observations, in that the higher the flux density is, the closer the turning point lies to the limb. There is a tendency, however, for the maximum to be reached closer to the limb when determined from two vantage points. We note that due to the preliminary nature of this study, these results must be taken with caution. Conclusions. 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L.</creatorcontrib><creatorcontrib>Gizon, L.</creatorcontrib><creatorcontrib>Grauf, B.</creatorcontrib><creatorcontrib>Heerlein, K.</creatorcontrib><creatorcontrib>Korpi-Lagg, A.</creatorcontrib><creatorcontrib>Lange, T.</creatorcontrib><creatorcontrib>López Jiménez, A.</creatorcontrib><creatorcontrib>Maue, T.</creatorcontrib><creatorcontrib>Meller, R.</creatorcontrib><creatorcontrib>Müller, R.</creatorcontrib><creatorcontrib>Nakai, E.</creatorcontrib><creatorcontrib>Schmidt, W.</creatorcontrib><creatorcontrib>Schou, J.</creatorcontrib><creatorcontrib>Sinjan, J.</creatorcontrib><creatorcontrib>Staub, J.</creatorcontrib><creatorcontrib>Strecker, H.</creatorcontrib><creatorcontrib>Torralbo, I.</creatorcontrib><creatorcontrib>Valori, G.</creatorcontrib><collection>CrossRef</collection><jtitle>Astronomy and astrophysics (Berlin)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Albert, K.</au><au>Krivova, N. A.</au><au>Hirzberger, J.</au><au>Solanki, S. K.</au><au>Moreno Vacas, A.</au><au>Orozco Suárez, D.</au><au>Albelo Jorge, N.</au><au>Appourchaux, T.</au><au>Alvarez-Herrero, A.</au><au>Blanco Rodríguez, J.</au><au>Gandorfer, A.</au><au>Gutierrez-Marques, P.</au><au>Kahil, F.</au><au>Kolleck, M.</au><au>Volkmer, R.</au><au>del Toro Iniesta, J. C.</au><au>Woch, J.</au><au>Fiethe, B.</au><au>Pérez-Grande, I.</au><au>Sanchis Kilders, E.</au><au>Balaguer Jiménez, M.</au><au>Bellot Rubio, L. R.</au><au>Calchetti, D.</au><au>Carmona, M.</au><au>Deutsch, W.</au><au>Feller, A.</au><au>Fernandez-Rico, G.</au><au>Fernández-Medina, A.</au><au>García Parejo, P.</au><au>Gasent Blesa, J. L.</au><au>Gizon, L.</au><au>Grauf, B.</au><au>Heerlein, K.</au><au>Korpi-Lagg, A.</au><au>Lange, T.</au><au>López Jiménez, A.</au><au>Maue, T.</au><au>Meller, R.</au><au>Müller, R.</au><au>Nakai, E.</au><au>Schmidt, W.</au><au>Schou, J.</au><au>Sinjan, J.</au><au>Staub, J.</au><au>Strecker, H.</au><au>Torralbo, I.</au><au>Valori, G.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Intensity contrast of solar network and faculae close to the solar limb, observed from two vantage points</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2023-10-01</date><risdate>2023</risdate><volume>678</volume><spage>A163</spage><pages>A163-</pages><issn>0004-6361</issn><eissn>1432-0746</eissn><abstract>Context. The brightness of faculae and network depends on the angle at which they are observed and the magnetic flux density. Close to the limb, the assessment of this relationship has until now been hindered by the increasingly lower signal in magnetograms. Aims. This preliminary study aims to highlight the potential of using simultaneous observations from different vantage points to better determine the properties of faculae close to the limb. Methods. We used data from the Solar Orbiter/Polarimetric and Helioseismic Imager (SO/PHI), and the Solar Dynamics Observatory/Helioseismic and Magnetic Imager (SDO/HMI), recorded at an ∼60° angular separation of their lines of sight at the Sun. We used the continuum intensity observed close to the limb by SO/PHI and complemented it with the co-observed B LOS from SDO/HMI, originating closer to disc centre (as seen by SDO/HMI), thus avoiding the degradation of the magnetic field signal near the limb. Results. We derived the dependence of facular brightness in the continuum on disc position and magnetic flux density from the combined observations of SO/PHI and SDO/HMI. Compared with a single point of view, we were able to obtain contrast values reaching closer to the limb and to lower field strengths. We find the general dependence of the limb distance at which the contrast is maximum on the flux density to be at large in line with single viewpoint observations, in that the higher the flux density is, the closer the turning point lies to the limb. There is a tendency, however, for the maximum to be reached closer to the limb when determined from two vantage points. We note that due to the preliminary nature of this study, these results must be taken with caution. Conclusions. Our analysis shows that studies involving two viewpoints can significantly improve the detection of faculae near the solar limb and the determination of their brightness contrast relative to the quiet Sun.</abstract><doi>10.1051/0004-6361/202346037</doi><orcidid>https://orcid.org/0000-0001-8829-1938</orcidid><orcidid>https://orcid.org/0000-0002-2391-6156</orcidid><orcidid>https://orcid.org/0000-0001-9358-5834</orcidid><orcidid>https://orcid.org/0000-0002-3418-8449</orcidid><orcidid>https://orcid.org/0000-0002-7336-0926</orcidid><orcidid>https://orcid.org/0000-0002-5387-636X</orcidid><orcidid>https://orcid.org/0000-0002-1377-3067</orcidid><orcidid>https://orcid.org/0000-0002-3387-026X</orcidid><orcidid>https://orcid.org/0000-0002-1225-4177</orcidid><orcidid>https://orcid.org/0000-0002-3776-9548</orcidid><orcidid>https://orcid.org/0000-0001-9228-3412</orcidid><orcidid>https://orcid.org/0000-0002-4792-1144</orcidid><orcidid>https://orcid.org/0000-0002-9972-9840</orcidid><orcidid>https://orcid.org/0000-0003-1459-7074</orcidid><orcidid>https://orcid.org/0000-0003-1483-4535</orcidid><orcidid>https://orcid.org/0000-0001-7696-8665</orcidid><orcidid>https://orcid.org/0000-0002-1232-4315</orcidid><orcidid>https://orcid.org/0000-0002-7145-2835</orcidid><orcidid>https://orcid.org/0000-0003-2755-5295</orcidid><orcidid>https://orcid.org/0000-0001-7809-0067</orcidid><orcidid>https://orcid.org/0000-0001-9272-6439</orcidid><orcidid>https://orcid.org/0000-0001-8669-8857</orcidid><oa>free_for_read</oa></addata></record>
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title Intensity contrast of solar network and faculae close to the solar limb, observed from two vantage points
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