Sunspots: An overview

By S. Solanki. 2003

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In Astronomy and Astrophysics

Citations in the corpus

Rotation periods of 12 000 main-sequence Kepler stars: Dependence on stellar spectral type and comparison with v sin i observations (2013, background): “Sunspots and solar active regions have lifetimes of days to weeks (rarely months) (Solanki 2003) and are reasonably good tracers of solar surface rotation at low latitudes.”
Impulsive Phase Flare Energy Transport by Large-Scale Alfvén Waves and the Electron Acceleration Problem (2007, background): “A large sunspot may have a size scale of some 3 ; 104 km, an umbral field of a few ; 0:1 T, and an outer penumbral field of 0.08–0.17 T (Solanki 2003).”
Reconstruction of total and spectral solar irradiance from 1974 to 2013 based on KPVT, SoHO/MDI and SDO/HMI observations (2014, methodology): “In both instances, the umbral threshold (0.70 for KPSPM and 0.64 for MDI) was set at the level that produced an umbra to sunspot area ra- tio of 0.2 (a level consistent with observations, Solanki 2003; Wenzler 2005).”
The Solar Optical Telescope for the Hinode Mission: An Overview (2007, background): “The magnetic field in the photosphere is distributed in a very inhomogeneous way, 1-4 with sunspots and faculae being the centerpieces of active regions (Solanki, 2003; Weiss, 2006; Ferriz-Mas and Steiner, 2008).”
Disentangling the Planet from the Star in Late-Type M Dwarfs: A Case Study of TRAPPIST-1g (2018, background): “This translates to a spot size within the transit chord with a physical radii of ≤ 1.22 megameters (Mm); in contrast the smallest spots on the Sun are ∼1.75 Mm (Solanki 2003).”
The magnetic field in the solar atmosphere (2014, background): “site polarity (Nakagawa et al., 1971; Woodard and Chae, 1999), allowing a mass ﬂow away from the spot (Evershed, 1909) or into the spot (“inverse Evershed eect”; St. John, 1913, and for a review see Solanki (2003)). In a similar fashion, ﬁbrils (seen, e.g., in H) are thought to connect opposite pola”
The Sun’s Supergranulation (2010, background): “…is concerned, many studies in the past have focused on the detection and characterisation of intrinsic flows associated with sunspot regions (see Solanki (2003) and Thomas and Weiss (2008) for exhaustive descriptions of sunspot structure and dynamics) and significant observational progress has…”
The Polarimetric and Helioseismic Imager on Solar Orbiter (2019, background): “Similarly, the solar surface is depressed in magnetic structures such as faculae, pores and sunspots, with the difference in height to the surface in the quiet Sun being called the Wilson depression (see, e.g. the review by Solanki 2003).”
DETECTING PLANETS AROUND VERY LOW MASS STARS WITH THE RADIAL VELOCITY METHOD (2009, background): “The coolest temperatures in large sunspots can be ∼ 2000K lower than the temperature in the surrounding photosphere (Solanki 2003).”
An Efficient Algorithm for Automatic Peak Detection in Noisy Periodic and Quasi-Periodic Signals (2012, background): “The time series analyzed comprises the total monthly number of sunspots, i.e. , the number of dark spots on the solar surface caused by interactions between the solar magnetic field and the Sun’s plasma [42].”
Local Helioseismology: Three-Dimensional Imaging of the Solar Interior (2010, background): “Recent reviews about sunspots are provided by, e.g., Solanki (2003) and Moradi et al. (2009, submitted).”
Solar Surface Magnetism and Irradiance on Time Scales from Days to the 11-Year Cycle (2009, background): “Magnetic field strengths up to 6 kG (in an extreme case) are found in the photosphere, see Solanki (2003), Livingston et al. (2006) for distribution of sunspot magnetic fields, and Abramenko and Longcope (2005) for active region magnetic fields.”
Solar Irradiance Variability and Climate (2013, background): “…that often have dimensions of multiple 10 Mm. Sunspots, forming the hearts of active regions, clearly are dark (see Rempel & Schlichenmaier 2011, Solanki 2003 for reviews), while the small magnetic elements that populate (and form) the faculae in active regions and the network elsewhere on the…”
Reconstruction of solar total irradiance since 1700 from the surface magnetic flux (2007, result): “We use a fixed ratio between umbral and penumbral areas, αu/(αu + αp) = 0.2 as obtained by Wenzler (2005) for recent cycles and in agreement with other estimates reported in the literature (for an overview see Solanki 2003).”
Magnetic Fields of Nondegenerate Stars (2009, background): “We know for instance that the magnetic field of the Sun is highly complex, giving rise not only to sunspot (e.g., Solanki 2003) but also to a complex set of magnetic features of smaller sizes such as ephemeral regions, bright poin s r inter-network fields (e.g., Stenflo 1989; Lites et al. 2008).”
Reconstruction of solar irradiance variations in cycles 21-23 based on surface magnetic fields (2006, background): “In reality, however, pores are closer in brightness to sunspot penumbra than to umbrae and small sunspots are not as dark as large spots (Collados et al. 1994; cf. Solanki 2003).”