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Journal articles on the topic 'Coronal holes (Astronomy)'

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Published: 4 June 2021
Last updated: 7 February 2022

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1

Parker, E. N. "Heating solar coronal holes." Astrophysical Journal 372 (May 1991): 719. http://dx.doi.org/10.1086/170015.

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2

Fainshtein, V. G., and G. V. Rudenko. "The birth of coronal holes." Proceedings of the International Astronomical Union 2004, IAUS223 (June 2004): 379–80. http://dx.doi.org/10.1017/s1743921304006192.

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3

Gopasyuk, O. S., E. A. Baranovskii, V. P. Tarashchuk, and N. I. Shtertser. "Physical Conditions in Coronal Holes." Astrophysics 63, no. 3 (September 2020): 421–29. http://dx.doi.org/10.1007/s10511-020-09646-z.

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4

Sakurai, Takashi. "Cyclical variation of the quiet corona and coronal holes." Journal of Astrophysics and Astronomy 21, no. 3-4 (September 2000): 389–95. http://dx.doi.org/10.1007/bf02702431.

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5

Mazumder, Rakesh, Prantika Bhowmik, and Dibyendu Nandy. "Properties of Coronal Holes in Solar Cycle 21-23 using McIntosh archive." Proceedings of the International Astronomical Union 13, S340 (February 2018): 187–88. http://dx.doi.org/10.1017/s1743921318001394.

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AbstractWe study the properties of coronal holes during solar cycle 21-23 from the McIntosh archive. In the spatial distribution of coronal hole area we find that there is a sharp increase in coronal hole area at high latitude in agreement with expected open flux configuration there. In overall spatiotemporal distribution of coronal hole centroids, we find the dominance of high latitude coronal holes except for the maximum of the solar cycle, when coronal holes mostly appear in low latitudes. This is in agreement with the expected solar cycle evolution of surface magnetic flux.
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6

Inglis, A. R., R. E. O’Connor, W. D. Pesnell, M. S. Kirk, and N. Karna. "Characteristics of Ephemeral Coronal Holes." Astrophysical Journal 880, no. 2 (July 30, 2019): 98. http://dx.doi.org/10.3847/1538-4357/ab27c1.

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7

Neutsch, Wolfram, and Horst Fichtner. "Coronal holes and icosahedral symmetry." Solar Physics 115, no. 1 (1988): 161–69. http://dx.doi.org/10.1007/bf00146237.

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8

Kalisch, Herbert, Wolfram Neutsch, Horst Fichtner, S. Ranga Sreenivasan, and Maurice Shevalier. "Coronal holes and icosahedral symmetry." Astrophysics and Space Science 288, no. 4 (2003): 547–71. http://dx.doi.org/10.1023/b:astr.0000005090.40916.d1.

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9

Neutsch, Wolfram, Herbert Kalisch, Horst Fichtner, S. Ranga Sreenivasan, and Maurice Shevalier. "Coronal Holes and Icosahedral Symmetry." Astrophysics and Space Science 288, no. 3 (2003): 391–408. http://dx.doi.org/10.1023/b:astr.0000006063.08122.12.

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10

Scullion, E., M. D. Popescu, D. Banerjee, J. G. Doyle, and R. Erdélyi. "JETS IN POLAR CORONAL HOLES." Astrophysical Journal 704, no. 2 (October 1, 2009): 1385–95. http://dx.doi.org/10.1088/0004-637x/704/2/1385.

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11

Shelke, Rajendra N., and M. C. Pande. "Differential rotation of coronal holes." Solar Physics 95, no. 1 (January 1985): 193–97. http://dx.doi.org/10.1007/bf00162647.

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12

Baranovskii, E. A., O. S. Gopasyuk, and N. I. Shtertser. "Coronal Holes According to Chromospheric Observations." Astrophysics 62, no. 2 (May 10, 2019): 226–33. http://dx.doi.org/10.1007/s10511-019-09576-5.

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13

Karachik, Nina V., and Alexei A. Pevtsov. "SOLAR WIND AND CORONAL BRIGHT POINTS INSIDE CORONAL HOLES." Astrophysical Journal 735, no. 1 (June 15, 2011): 47. http://dx.doi.org/10.1088/0004-637x/735/1/47.

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14

Hofmeister, Stefan J., Dominik Utz, Stephan G. Heinemann, Astrid Veronig, and Manuela Temmer. "Photospheric magnetic structure of coronal holes." Astronomy & Astrophysics 629 (August 28, 2019): A22. http://dx.doi.org/10.1051/0004-6361/201935918.

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In this study, we investigate in detail the photospheric magnetic structure of 98 coronal holes using line-of-sight magnetograms of SDO/HMI, and for a subset of 42 coronal holes using HINODE/SOT G-band filtergrams. We divided the magnetic field maps into magnetic elements and quiet coronal hole regions by applying a threshold at ±25 G. We find that the number of magnetic bright points in magnetic elements is well correlated with the area of the magnetic elements (cc = 0.83 ± 0.01). Further, the magnetic flux of the individual magnetic elements inside coronal holes is related to their area by a power law with an exponent of 1.261 ± 0.004 (cc = 0.984 ± 0.001). Relating the magnetic elements to the overall structure of coronal holes, we find that on average (69 ± 8)% of the overall unbalanced magnetic flux of the coronal holes arises from long-lived magnetic elements with lifetimes > 40 h. About (22 ± 4)% of the unbalanced magnetic flux arises from a very weak background magnetic field in the quiet coronal hole regions with a mean magnetic field density of about 0.2−1.2 G. This background magnetic field is correlated to the flux of the magnetic elements with lifetimes of > 40 h (cc = 0.88 ± 0.02). The remaining flux arises from magnetic elements with lifetimes < 40 h. By relating the properties of the magnetic elements to the overall properties of the coronal holes, we find that the unbalanced magnetic flux of the coronal holes is completely determined by the total area that the long-lived magnetic elements cover (cc = 0.994 ± 0.001).
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15

Bhatnagar, Arvind. "Solar mass ejections and coronal holes." Astrophysics and Space Science 243, no. 1 (1996): 105–12. http://dx.doi.org/10.1007/bf00644039.

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16

Wang, Y. M., and N. R. ,. Jr Sheeley. "Understanding the rotation of coronal holes." Astrophysical Journal 414 (September 1993): 916. http://dx.doi.org/10.1086/173135.

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17

Young, Peter R. "DARK JETS IN SOLAR CORONAL HOLES." Astrophysical Journal 801, no. 2 (March 12, 2015): 124. http://dx.doi.org/10.1088/0004-637x/801/2/124.

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18

Molodenskiĭ, M. M., and L. I. Starkova. "Solar structures related to coronal holes." Astronomy Reports 51, no. 12 (December 2007): 1036–41. http://dx.doi.org/10.1134/s1063772907120074.

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19

Wang, Y. M. "Coronal Holes and Open Magnetic Flux." Space Science Reviews 144, no. 1-4 (September 23, 2008): 383–99. http://dx.doi.org/10.1007/s11214-008-9434-0.

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20

Banerjee, D., G. R. Gupta, and L. Teriaca. "Propagating MHD Waves in Coronal Holes." Space Science Reviews 158, no. 2-4 (November 3, 2010): 267–88. http://dx.doi.org/10.1007/s11214-010-9698-z.

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21

Insley, J. E., V. Moore, and R. A. Harrison. "The differential rotation of the corona as indicated by coronal holes." Solar Physics 160, no. 1 (August 1995): 1–18. http://dx.doi.org/10.1007/bf00679089.

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22

Sulistiani, Santi, and Dhani Herdiwijaya. "Solar coronal holes and their geo-effectiveness." Journal of Physics: Conference Series 1127 (January 2019): 012052. http://dx.doi.org/10.1088/1742-6596/1127/1/012052.

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23

Heinemann, S. G., V. Jerčić, M. Temmer, S. J. Hofmeister, M. Dumbović, S. Vennerstrom, G. Verbanac, and A. M. Veronig. "A statistical study of the long-term evolution of coronal hole properties as observed by SDO." Astronomy & Astrophysics 638 (June 2020): A68. http://dx.doi.org/10.1051/0004-6361/202037613.

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Context. Understanding the evolution of coronal holes is especially important when studying the high-speed solar wind streams that emanate from them. Slow- and high-speed stream interaction regions may deliver large amounts of energy into the Earth’s magnetosphere-ionosphere system, cause geomagnetic storms, and shape interplanetary space. Aims. By statistically investigating the long-term evolution of well-observed coronal holes we aim to reveal processes that drive the observed changes in the coronal hole parameters. By analyzing 16 long-living coronal holes observed by the Solar Dynamic Observatory, we focus on coronal, morphological, and underlying photospheric magnetic field characteristics, and investigate the evolution of the associated high-speed streams. Methods. We use the Collection of Analysis Tools for Coronal Holes to extract and analyze coronal holes using 193 Å EUV observations taken by the Atmospheric Imaging Assembly as well as line–of–sight magnetograms observed by the Helioseismic and Magnetic Imager. We derive changes in the coronal hole properties and look for correlations with coronal hole evolution. Further, we analyze the properties of the high–speed stream signatures near 1AU from OMNI data by manually extracting the peak bulk velocity of the solar wind plasma. Results. We find that the area evolution of coronal holes shows a general trend of growing to a maximum followed by a decay. We did not find any correlation between the area evolution and the evolution of the signed magnetic flux or signed magnetic flux density enclosed in the projected coronal hole area. From this we conclude that the magnetic flux within the extracted coronal hole boundaries is not the main cause for its area evolution. We derive coronal hole area change rates (growth and decay) of (14.2 ± 15.0)×108 km2 per day showing a reasonable anti-correlation (ccPearson = −0.48) to the solar activity, approximated by the sunspot number. The change rates of the signed mean magnetic flux density (27.3 ± 32.2 mG day−1) and the signed magnetic flux (30.3 ± 31.5 1018 Mx day−1) were also found to be dependent on solar activity (ccPearson = 0.50 and ccPearson = 0.69 respectively) rather than on the individual coronal hole evolutions. Further we find that the relation between coronal hole area and high-speed stream peak velocity is valid for each coronal hole over its evolution, but we see significant variations in the slopes of the regression lines.
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24

Bilenko, I. A. "Formation and evolution of different type coronal holes." Proceedings of the International Astronomical Union 2004, IAUS223 (June 2004): 373–74. http://dx.doi.org/10.1017/s1743921304006167.

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25

Obridko, V. N., and B. D. Shelting. "Coronal holes as indicators of large-scale magnetic fields in the corona." Solar Physics 124, no. 1 (1989): 73–80. http://dx.doi.org/10.1007/bf00146520.

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26

Wilhelm, Klaus, Eckart Marsch, Bhola N. Dwivedi, Donald M. Hassler, Philippe Lemaire, Alan H. Gabriel, and Martin C. E. Huber. "The Solar Corona above Polar Coronal Holes as Seen by SUMER onSOHO." Astrophysical Journal 500, no. 2 (June 20, 1998): 1023–38. http://dx.doi.org/10.1086/305756.

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27

Krista, Larisza D., Scott W. McIntosh, and Robert J. Leamon. "The Longitudinal Evolution of Equatorial Coronal Holes." Astronomical Journal 155, no. 4 (March 16, 2018): 153. http://dx.doi.org/10.3847/1538-3881/aaaebf.

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28

Meunier, N. "Large-scale photospheric dynamics below coronal holes." Astronomy & Astrophysics 443, no. 1 (October 21, 2005): 309–17. http://dx.doi.org/10.1051/0004-6361:20053249.

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29

Pascoe, D. J., V. M. Nakariakov, and E. G. Kupriyanova. "Fast magnetoacoustic wave trains in coronal holes." Astronomy & Astrophysics 568 (August 2014): A20. http://dx.doi.org/10.1051/0004-6361/201423931.

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30

Ofman, Leon. "MHD Waves and Heating in Coronal Holes." Space Science Reviews 120, no. 1-2 (September 2005): 67–94. http://dx.doi.org/10.1007/s11214-005-5098-1.

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31

Das, T. K., T. N. Chatterjee, and A. K. Sen. "Solar cycle dependence of polar coronal holes." Solar Physics 148, no. 1 (November 1993): 61–64. http://dx.doi.org/10.1007/bf00675535.

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32

Gopalswamy, N., K. Shibasaki, and M. Salem. "Microwave enhancement in coronal holes: Statistical properties." Journal of Astrophysics and Astronomy 21, no. 3-4 (September 2000): 413–17. http://dx.doi.org/10.1007/bf02702435.

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33

Jarolim, R., A. M. Veronig, S. Hofmeister, S. G. Heinemann, M. Temmer, T. Podladchikova, and K. Dissauer. "Multi-channel coronal hole detection with convolutional neural networks." Astronomy & Astrophysics 652 (August 2021): A13. http://dx.doi.org/10.1051/0004-6361/202140640.

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Context. A precise detection of the coronal hole boundary is of primary interest for a better understanding of the physics of coronal holes, their role in the solar cycle evolution, and space weather forecasting. Aims. We develop a reliable, fully automatic method for the detection of coronal holes that provides consistent full-disk segmentation maps over the full solar cycle and can perform in real-time. Methods. We use a convolutional neural network to identify the boundaries of coronal holes from the seven extreme ultraviolet (EUV) channels of the Atmospheric Imaging Assembly (AIA) and from the line-of-sight magnetograms provided by the Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO). For our primary model (Coronal Hole RecOgnition Neural Network Over multi-Spectral-data; CHRONNOS) we use a progressively growing network approach that allows for efficient training, provides detailed segmentation maps, and takes into account relations across the full solar disk. Results. We provide a thorough evaluation for performance, reliability, and consistency by comparing the model results to an independent manually curated test set. Our model shows good agreement to the manual labels with an intersection-over-union (IoU) of 0.63. From the total of 261 coronal holes with an area > 1.5 × 1010 km2 identified during the time-period from November 2010 to December 2016, 98.1% were correctly detected by our model. The evaluation over almost the full solar cycle no. 24 shows that our model provides reliable coronal hole detections independent of the level of solar activity. From a direct comparison over short timescales of days to weeks, we find that our model exceeds human performance in terms of consistency and reliability. In addition, we train our model to identify coronal holes from each channel separately and show that the neural network provides the best performance with the combined channel information, but that coronal hole segmentation maps can also be obtained from line-of-sight magnetograms alone. Conclusions. The proposed neural network provides a reliable data set for the study of solar-cycle dependencies and coronal-hole parameters. Given the fast and robust coronal hole segmentation, the algorithm is also highly suitable for real-time space weather applications.
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34

Petrie, G. J. D., and K. J. Haislmaier. "LOW-LATITUDE CORONAL HOLES, DECAYING ACTIVE REGIONS, AND GLOBAL CORONAL MAGNETIC STRUCTURE." Astrophysical Journal 775, no. 2 (September 11, 2013): 100. http://dx.doi.org/10.1088/0004-637x/775/2/100.

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35

Nikolić, Ljubomir. "PFSS-Based Solar Wind Forecast and the Radius of the Source-Surface." Proceedings of the International Astronomical Union 13, S335 (July 2017): 307–9. http://dx.doi.org/10.1017/s1743921317009875.

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AbstractThe potential-field source-surface (PFSS) model of the solar corona is a widely used tool in the space weather research and operations. In particular, the PFSS model is used in solar wind forecast models which empirically associate solar wind properties with the numerically derived coronal magnetic field. In the PFSS model, the spherical surface where magnetic field lines are forced to open is typically placed at 2.5 solar radii. However, the results presented here suggest that setting this surface (the source-surface) to lower heights can provide a better agreement between observed and modelled coronal holes during the current solar cycle. Furthermore, the lower heights of the source-surface provide a better match between observed and forecasted solar wind speed.
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36

Nisticò, G., V. Bothmer, S. Patsourakos, and G. Zimbardo. "Observational features of equatorial coronal hole jets." Annales Geophysicae 28, no. 3 (March 1, 2010): 687–96. http://dx.doi.org/10.5194/angeo-28-687-2010.

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Abstract. Collimated ejections of plasma called "coronal hole jets" are commonly observed in polar coronal holes. However, such coronal jets are not only a specific features of polar coronal holes but they can also be found in coronal holes appearing at lower heliographic latitudes. In this paper we present some observations of "equatorial coronal hole jets" made up with data provided by the STEREO/SECCHI instruments during a period comprising March 2007 and December 2007. The jet events are selected by requiring at least some visibility in both COR1 and EUVI instruments. We report 15 jet events, and we discuss their main features. For one event, the uplift velocity has been determined as about 200 km s−1, while the deceleration rate appears to be about 0.11 km s−2, less than solar gravity. The average jet visibility time is about 30 min, consistent with jet observed in polar regions. On the basis of the present dataset, we provisionally conclude that there are not substantial physical differences between polar and equatorial coronal hole jets.
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37

Landi, E., and S. R. Cranmer. "ION TEMPERATURES IN THE LOW SOLAR CORONA: POLAR CORONAL HOLES AT SOLAR MINIMUM." Astrophysical Journal 691, no. 1 (January 19, 2009): 794–805. http://dx.doi.org/10.1088/0004-637x/691/1/794.

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38

Panesar, Navdeep K., Alphonse C. Sterling, and Ronald L. Moore. "Magnetic Flux Cancelation as the Trigger of Solar Coronal Jets in Coronal Holes." Astrophysical Journal 853, no. 2 (February 5, 2018): 189. http://dx.doi.org/10.3847/1538-4357/aaa3e9.

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39

Piantschitsch, Isabell, Bojan Vršnak, Arnold Hanslmeier, Birgit Lemmerer, Astrid Veronig, Aaron Hernandez-Perez, Jaša Čalogović, and Tomislav Žic. "A Numerical Simulation of Coronal Waves Interacting with Coronal Holes. I. Basic Features." Astrophysical Journal 850, no. 1 (November 20, 2017): 88. http://dx.doi.org/10.3847/1538-4357/aa8cc9.

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40

Piantschitsch, I., and J. Terradas. "Geometrical properties of the interaction between oblique incoming coronal waves and coronal holes." Astronomy & Astrophysics 651 (July 2021): A67. http://dx.doi.org/10.1051/0004-6361/202040182.

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Observations of coronal waves (CWs) interacting with coronal holes (CHs) show the formation of typical wave-like features, such as reflected, refracted and transmitted waves (collectively, secondary waves). In accordance with these observations, numerical evidence for the wave characteristics of CWs is given by simulations, which demonstrate effects of deflection and reflection when a CW interacts with regions exhibiting a sudden density drop, such as CHs. However, secondary waves are usually weak in their signal and simulations are limited in the way the according idealisations have to be chosen. Hence, several properties of the secondary waves during a CW–CH interaction are unclear or ambiguous and might lead to misinterpretations. In this study we follow a theoretical approach and focus in particular on the geometrical properties of secondary waves caused by the interaction between oblique incoming CWs and CHs. Based on a linear theory, we derive analytical expressions for reflection and transmission coefficients, which tell us how strongly the amplitudes of the secondary waves increase and decrease with respect to the incoming wave, respectively. Additionally, we provide analytical terms for crucial incidence angles that are capable of giving information about the energy flux, the phase and the reflection properties of the secondary waves. These novel expressions provide a supplementary tool for estimating CW properties in a fast and straightforward way, and therefore might have relevant consequences for a possible new interpretation of previously studied CW–CH interaction events and may help in the clarification of ambiguous observational data.
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41

Harden, Abigail R., Navdeep K. Panesar, Ronald L. Moore, Alphonse C. Sterling, and Mitzi L. Adams. "What Causes Faint Solar Coronal Jets from Emerging Flux Regions in Coronal Holes?" Astrophysical Journal 912, no. 2 (May 1, 2021): 97. http://dx.doi.org/10.3847/1538-4357/abee19.

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42

Sasso, C., R. F. Pinto, V. Andretta, R. A. Howard, A. Vourlidas, A. Bemporad, S. Dolei, et al. "Comparing extrapolations of the coronal magnetic field structure at 2.5R⊙with multi-viewpoint coronagraphic observations." Astronomy & Astrophysics 627 (June 25, 2019): A9. http://dx.doi.org/10.1051/0004-6361/201834125.

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The magnetic field shapes the structure of the solar corona, but we still know little about the interrelationships between the coronal magnetic field configurations and the resulting quasi-stationary structures observed in coronagraphic images (such as streamers, plumes, and coronal holes). One way to obtain information on the large-scale structure of the coronal magnetic field is to extrapolate it from photospheric data and compare the results with coronagraphic images. Our aim is to verify whether this comparison can be a fast method to systematically determine the reliability of the many methods that are available for modeling the coronal magnetic field. Coronal fields are usually extrapolated from photospheric measurements that are typically obtained in a region close to the central meridian on the solar disk and are then compared with coronagraphic images at the limbs, acquired at least seven days before or after to account for solar rotation. This implicitly assumes that no significant changes occurred in the corona during that period. In this work, we combine images from three coronagraphs (SOHO/LASCO-C2 and the two STEREO/SECCHI-COR1) that observe the Sun from different viewing angles to build Carrington maps that cover the entire corona to reduce the effect of temporal evolution to about five days. We then compare the position of the observed streamers in these Carrington maps with that of the neutral lines obtained from four different magnetic field extrapolations to evaluate the performances of the latter in the solar corona. Our results show that the location of coronal streamers can provide important indications to distinguish between different magnetic field extrapolations.
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43

Neugebauer, M. "Observations of the solar wind from coronal holes." Space Science Reviews 70, no. 1-2 (October 1994): 319–30. http://dx.doi.org/10.1007/bf00777887.

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44

Bravo, S., and G. A. Stewart. "Fast and Slow Wind from Solar Coronal Holes." Astrophysical Journal 489, no. 2 (November 10, 1997): 992–99. http://dx.doi.org/10.1086/304789.

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45

Murawski, K., R. Oliver, and J. L. Ballester. "Nonlinear fast magnetosonic waves in solar coronal holes." Astronomy & Astrophysics 375, no. 1 (August 2001): 264–74. http://dx.doi.org/10.1051/0004-6361:20010869.

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46

Bilenko, Irina A. "Longitudinal Distribution of Coronal Holes During 1976–2002." Solar Physics 221, no. 2 (June 2004): 261–82. http://dx.doi.org/10.1023/b:sola.0000035067.88819.40.

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47

Nash, A. G., N. R. Sheeley, and Y. M. Wang. "Mechanisms for the rigid rotation of coronal holes." Solar Physics 117, no. 2 (September 1988): 359–89. http://dx.doi.org/10.1007/bf00147253.

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48

Teplitskaya, R. B., I. P. Turova, and O. A. Ozhogina. "Intensity oscillations at the feet of coronal holes." Astronomy Letters 35, no. 10 (October 2009): 712–22. http://dx.doi.org/10.1134/s1063773709100089.

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49

Wang, Y. ‐M, and N. R. Sheeley, Jr. "Footpoint Switching and the Evolution of Coronal Holes." Astrophysical Journal 612, no. 2 (September 10, 2004): 1196–205. http://dx.doi.org/10.1086/422711.

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50

Das, T. K., T. N. Chatterji, T. Roy, and A. K. Sen. "Sixty six day periodicity of polar coronal holes." Astrophysics and Space Science 213, no. 2 (1994): 327–30. http://dx.doi.org/10.1007/bf00658219.

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