Evolution of the flow field in decaying active regions, Transition from a moat flow to a supergranular flow

We investigate the evolution of the horizontal flow field around sunspots during their decay by analysing its extension and horizontal velocity around eight spots using SDO/HMI Doppler maps. By assuming a radially symmetrical flow field, the applied analysis method determines the radial dependence of the azimuthally averaged flow field. For comparison, we studied the flow in supergranules using the same technique. All investigated, fully fledged sunspots are surrounded by a flow field whose horizontal velocity profile decreases continuously from 881 m s$^{-1}$ at 1.1 Mm off the spot boundary, down to 199 m s$^{-1}$ at a mean distance of 11.9 Mm to that boundary. Once the penumbra is fully dissolved, however, the velocity profile of the flow changes: The horizontal velocity increases with increasing distance to the spot boundary until a maximum value of about 398 m s$^{-1}$ is reached. Then, the horizontal velocity decreases for farther distances to the spot boundary. In supergranules, the horizontal velocity increases with increasing distance to their centre up to a mean maximum velocity of 355 m s$^{-1}$. For larger distances, the horizontal velocity decreases. We thus find that the velocity profile of naked sunspots resembles that of supergranular flows. The evolution of the flow field around individual sunspots is influenced by the way the sunspot decays and by the interplay with the surrounding flow areas. Observations of the flow around eight decaying sunspots suggest that as long as penumbrae are present, sunspots with their moat cell are embedded in network cells. The disappearance of the penumbra (and consequently the moat flow) and the competing surrounding supergranular cells, both have a significant role in the evolution of the flow field: The moat cell transforms into a supergranule, which hosts the remaining naked spot.Comment: accepted for publication in A&A, 11 pages, 6 figures, 3 tables; appendix with 9 figures and 8 online movie

Magnetic properties of a long-lived sunspot - Vertical magnetic field at the umbral boundary

Context. In a recent statistical study of sunspots in 79 active regions, the vertical magnetic field component $B_\text{ver}$ averaged along the umbral boundary is found to be independent of sunspot size. The authors of that study conclude that the absolute value of $B_\text{ver}$ at the umbral boundary is the same for all spots. Aims. We investigate the temporal evolution of $B_\text{ver}$ averaged along the umbral boundary of one long-lived sunspot during its stable phase. Methods. We analysed data from the HMI instrument on-board SDO. Contours of continuum intensity at $I_\text{c}=0.5I_\text{qs}$, whereby $I_\text{qs}$ refers to the average over the quiet sun areas, are used to extract the magnetic field along the umbral boundary. Projection effects due to different formation heights of the Fe I 617.3 nm line and continuum are taken into account. To avoid limb artefacts, the spot is only analysed for heliocentric angles smaller than $60^{\circ}$. Results. During the first disc passage, NOAA AR 11591, $B_\text{ver}$ remains constant at 1693 G with a root-mean-square deviation of 15 G, whereas the magnetic field strength varies substantially (mean 2171 G, rms of 48 G) and shows a long term variation. Compensating for formation height has little influence on the mean value along each contour, but reduces the variations along the contour when away from disc centre, yielding a better match between the contours of $B_\text{ver}=1693$ G and $I_\text{c}=0.5I_\text{qs}$. Conclusions. During the disc passage of a stable sunspot, its umbral boundary can equivalently be defined by using the continuum intensity $I_\text{c}$ or the vertical magnetic field component $B_\text{ver}$. Contours of fixed magnetic field strength fail to outline the umbral boundary.Comment: accepted for publication in A&A; v2 minor edit, correcting statement regarding one citatio

Chromospheric impact of an exploding solar granule

Observations of multi-wavelength and therefore height-dependent information following events throughout the solar atmosphere and unambiguously assigning a relation between these rapidly evolving layers are rare and difficult to obtain. Yet, they are crucial for our understanding of the physical processes that couple the different regimes in the solar atmosphere. We characterize the exploding granule event with simultaneous observations of Hinode spectroplarimetric data in the solar photosphere and Hinode broadband CaIIH images combined with Interface Region Imaging Spectrograph (IRIS) slit spectra. We follow the evolution of an exploding granule and its connectivity throughout the atmosphere and analyze the dynamics of a magnetic element that has been affected by the abnormal granule. In addition to magnetic flux maps we use a local correlation tracking method to infer the horizontal velocity flows in the photosphere and apply a wavelet analysis on several IRIS chromospheric emission features such as MgIIk2v and MgIIk3 to detect oscillatory phenomena indicating wave propagation. During the vigorous expansion of the abnormal granule we detect radially outward horizontal flows, causing, together with the horizontal flows from the surrounding granules, the magnetic elements in the bordering intergranular lanes to be squeezed and elongated. In reaction to the squeezing, we detect a chromospheric intensity and velocity oscillation pulse which we identify as an upward traveling hot shock front propagating clearly through the IRIS spectral line diagnostics of MgIIh&k. Conclusion: Exploding granules can trigger upward-propagating shock fronts that dissipate in the chromosphere.Comment: 5 pages (3 figures)+1 page movie snapshots(2 figures), accepted in A&A letters, movies can be found at http://www.science-media.org/216 and http://www.science-media.org/21

Spectropolarimetry of sunspot penumbrae

Die vorliegende Arbeit beschäftigt sich mit der Beobachtung von Feinstrukturen der Penumbren von Sonnenflecken mittels hoher räumlicher Auflösung und Vorwärtsmodellierung. Unter Verwendung von Bildrekonstruktionstechniken in Kombination mit zweidimensionalen spektropolarimetrischen Bildern können Magnetogramme und Geschwindigkeitsverläufe mit einer Auflösung im Bereich von 0".4 erstellt werden. Die daraus erhaltenen Ergebnisse stimmen überein mit der Annahme tief liegender Strömungkanäle entlang des horizontalen magnetsichen Felds oder möglicherweise Strömungkanäle, die aus den sub-photosphärischen Schichten austreten und wieder eintauchen, vergleichbar einer "Meereschlange".Darüberhinaus werden weitere dynamische Phänomene, welche den Reichturm der in Penumbren ablaufenden Prozesse zeigen, diskutiert und einige neue nicht erwartete Eigenschaften aufgezeigt

The magnetic nature of umbra-penumbra boundary in sunspots

Sunspots are the longest-known manifestation of solar activity, and their magnetic nature has been known for more than a century. Despite this, the boundary between umbrae and penumbrae, the two fundamental sunspot regions, has hitherto been solely defined by an intensity threshold. Here, we aim at studying the magnetic nature of umbra-penumbra boundaries in sunspots of different sizes, morphologies, evolutionary stages, and phases of the solar cycle. We used a sample of 88 scans of the Hinode/SOT spectropolarimeter to infer the magnetic field properties in at the umbral boundaries. We defined these umbra-penumbra boundaries by an intensity threshold and performed a statistical analysis of the magnetic field properties on these boundaries. We statistically prove that the umbra-penumbra boundary in stable sunspots is characterised by an invariant value of the vertical magnetic field component: the vertical component of the magnetic field strength does not depend on the umbra size, its morphology, and phase of the solar cycle. With the statistical Bayesian inference, we find that the strength of the vertical magnetic field component is, with a likelihood of 99\%, in the range of 1849-1885 G with the most probable value of 1867 G. In contrast, the magnetic field strength and inclination averaged along individual boundaries are found to be dependent on the umbral size: the larger the umbra, the stronger and more horizontal the magnetic field at its boundary. The umbra and penumbra of sunspots are separated by a boundary that has hitherto been defined by an intensity threshold. We now unveil the empirical law of the magnetic nature of the umbra-penumbra boundary in stable sunspots: it is an invariant vertical component of the magnetic field.Comment: accepted as A&A lette

Critical Science Plan for the Daniel K. Inouye Solar Telescope (DKIST)

Open Access funding provided by the National Solar Observatory (NSO). The NSO is operated by the Association of Universities for Research in Astronomy, Inc., and is funded by the National Science Foundation.The National Science Foundation’s Daniel K. Inouye Solar Telescope (DKIST) will revolutionize our ability to measure, understand, and model the basic physical processes that control the structure and dynamics of the Sun and its atmosphere. The first-light DKIST images, released publicly on 29 January 2020, only hint at the extraordinary capabilities that will accompany full commissioning of the five facility instruments. With this Critical Science Plan (CSP) we attempt to anticipate some of what those capabilities will enable, providing a snapshot of some of the scientific pursuits that the DKIST hopes to engage as start-of-operations nears. The work builds on the combined contributions of the DKIST Science Working Group (SWG) and CSP Community members, who generously shared their experiences, plans, knowledge, and dreams. Discussion is primarily focused on those issues to which DKIST will uniquely contribute.Publisher PDFPeer reviewe