Explore the vast range of titles available.

The monthly mean sea level along the U.S. Mid‐Atlantic Coast varies seasonally, reaching a minimum in January and a maximum in September during the 1960–2020 period. However, this seasonal cycle has changed significantly on multi‐decadal timescales. In the last two decades, the annual minimum has shifted from January to February. The amplitude of seasonal changes increased by 65% from 14.16 cm in 1980–1999 to 23.16 cm in 2000–2020. Even more concerning, the maximum sea level in September rose by 82%, from 6.81 to 12.38 cm, potentially exacerbating coastal flooding over the past 20 years. A two‐layer ocean model effectively replicates both the phase and magnitude of the observed changes and attributes these shifts to changes in wind stress near the coast, with relatively minor influence from deep ocean forcing. Both alongshore and cross‐shore wind stress changes are found to contribute to changes in the sea level's seasonal cycle. Plain Language Summary Sea level height varies seasonally in response to external forces and internal processes. Along the U.S. Mid‐Atlantic Coast, it varies about 19 cm between the seasonal low in January/February and the high in September, according to observations from the past six decades. However, this seasonal cycle has changed markedly on decadal timescales. Between 2000 and 2020, the amplitude of seasonal sea level variation increased by more than 65% compared to the previous two decades. Our analysis suggests that changes in wind stress, especially in coastal areas, are the primary driver of these changes. Key Points The seasonal cycle of sea level along the Mid‐Atlantic Coast has undergone significant changes in the last 6 decades The main driver for changes in the seasonal cycle is wind stress along the coastal areas Influences from deep open ocean make only minor contributions to changes in the seasonal cycle

Due to the differences between regions, the regional economy is also affected by the development of the real economy and the environment in a specific region. Thus, it is necessary to predict the development potential of the regional economy to ensure the smooth operation of the economy. The continuous upgrading of technology enables the country to grasp the development trend of the regional economy more accurately than ever before. However, the existing prediction techniques still have large errors. Therefore, this paper constructed a prediction model based on data mining technology to predict the development potential of the regional economy to enhance the accuracy of predictive models. The experiments showed that the prediction accuracy of the prediction model constructed in this paper could reach 96.78%, which could provide an accurate reference for the development of the regional economy to ensure the stable development of the regional economy, and has important application value. This paper constructs a prediction model based on data mining (DM) technology to predict the development potential of the regional economy to enhance the accuracy of predictive models.

In this paper, we examine the seasonal and interannual to decadal variability of oceanic downwelling in the Beaufort Sea. The surface wind stress is the primary driver for variability in the upper Arctic Ocean and sea ice. The seasonal variability of the surface wind over the western Arctic is strongly influenced by a high sea level pressure center that emerges in the fall and diminishes in the summer. The wind stress and sea ice velocity are both anticyclonic from fall to spring and thus force an upwelling along the Alaskan and Canadian coast and downwelling in the interior Beaufort Sea. The upwelling and downwelling varied significantly on the interannual to decadal time scales from 1979 to 2006. There was no significant correlation between the upwelling/downwelling rate in the Beaufort Sea and the Arctic Oscillation index over this 28 year period. The coastal upwelling and interior downwelling in the Beaufort Sea had gradually intensified from 1979 to 2006. This change was almost entirely due to the increase in sea ice velocity according to three additional sensitivity calculations. The anticyclonic ice velocity over the western Arctic Ocean accelerated in the 28 year period, and the acceleration was not driven solely by the wind stress. The geostrophic wind condition was actually similar between 1979–1986 and 1997–2004. However, the ice velocity was much greater in the latter period. We hypothesize that the change in ice dynamics (thinner and less areal coverage) was responsible for the change of ice velocity.

Similar to the cases of anemone jets, two-sided loop solar jets can also be produced by either flux emergence from the solar interior or small-scale filament eruptions. Using high-quality data from the Solar Dynamics Observatory, we have analyzed a two-sided loop solar jet triggered by the eruption of a small filament. The jet occurred in a pre-existing big filament channel. The detailed processes involved in the eruption of the small filament, the interaction between the erupted filament and the big filament channel, and the launch of the two-sided loop jet are presented. The observations further revealed notable asymmetry between the two branches of the jet spire: the northeastern branch is narrow and short, while the southern branch is wide and long and accompanied by discernible untwisting motions. We explored the unique appearance of the jet by employing the method of local potential field extrapolation to calculate the coronal magnetic field configuration around the jet. The photospheric magnetic flux below the small filament underwent cancellation for approximately 7 hr before the filament eruption, and the negative flux near the southern footpoint of the filament decreased by about 56% during this interval. Therefore, we propose that the primary photospheric driver of the filament eruption and the associated two-sided loop jet in this event is flux cancellation rather than flux emergence.

Coronal bright points (CBPs) are typical small-scale coronal brightenings that consist of a bundle of miniature coronal loops. Using the ultrahigh-resolution coronal images from the Extreme Ultraviolet Imager on board Solar Orbiter, we report the first observational evidence of oscillatory magnetic reconnection at a CBP. The reconnection is characterized by two bursty phases defined by a reconnection reversal. In the first phase, a current sheet (C1) was found to form in front of an expanding loop of the bright point. Interestingly, C1 shortened to a null point during 10 minutes after reaching its maximum length (∼2.4 Mm). Less than 3 minutes later, a new current sheet (C2) was clearly seen to grow out from the null point, but along an orthogonal direction relative to C1. C2 reached a maximum length of ∼4 Mm in 10 minutes and then became short and invisible in the next few minutes as the reconnection declined. The magnetic reconnection is evidenced by the brightening, plasma flow, and temperature increase at the ends of both C1 and C2. No significant magnetic cancellation or emergence but gradual convergence occurred during the few hours before the reconnection underneath the CBP. The transition from C1 to C2 suggests the occurrence of coronal oscillatory reconnection, whereby the inflow and outflow regions in the first phase become the outflow and inflow regions in the second phase, respectively. It is further found that the oscillatory reconnection could slightly modulate the change in brightness of the CBP. We propose that oscillatory reconnection has the potential to continuously heat solar small-scale structures without destroying their overall magnetic configurations.

Different from the classical emerging-flux model for solar jets, recent studies proposed that the great majority of solar coronal jets are triggered by minifilament eruptions and two magnetic reconnection processes should take place during the course, named as external reconnection (breakout reconnection) and internal reconnection (flare reconnection). With the excellent data of the Solar Dynamics Observatory, we present the observational signatures of these two magnetic reconnection processes during a solar coronal jet that occurred in a huge coronal hole of northern hemisphere. The jet was triggered by the eruption of a minifilament that located at a coronal bright point in the coronal hole. Weak bidirectional outflows were observed when the erupting minifilament approached the ambient open field, ejecting along the triggered jet spire and the jet base simultaneously. In addition, a flare current sheet occurred after the eruption of the minifilament, connecting the jet spire and the jet bright point (or flare). We suggest the occurrence of the weak bidirectional outflows and the flare current sheet correspond to the external and the internal reconnections, respectively. Prior to the eruption of the minifilament and the jet, photospheric magnetic flux cancellation maintained for more than 7 hr in the source region, and the positive flux decreased for about 28.6% during this period. So, consistent with the recent observations, the trigger mechanism of the minifilament eruption and the following jet in this event may be flux cancellation rather than flux emergence.

Ocean circulation responds to seasonal and longer timescale changes in atmospheric forcing through the propagation of Rossby and boundary waves, which transmit pressure anomalies and influence geostrophic velocities along their pathways. Rossby waves are guided by potential vorticity isolines shaped by bathymetry. This study hypothesizes that seasonal velocity variability in the North Atlantic Ocean's deep water layer is primarily driven by wind stress and that its pattern and magnitude are strongly influenced by bathymetry. Analysis of satellite gravimetric observations, ocean state estimates, and wind‐driven model simulations reveals that Ocean Bottom Pressure (OBP) and velocity in the deep water layer are significantly modulated by bathymetry, with pronounced variability near topographic features. These findings suggest that measurements of the Deep Western Boundary Current alone may be insufficiently to fully capture the net variability of the Atlantic Meridional Overturning Circulation (AMOC). Plain Language Summary Ocean circulation changes with the seasons, and these changes are largely influenced by the shape of the seafloor. This happens because waves, called topographic Rossby waves, travel along pathways that are strongly influenced by bathymetry and carry information about pressure changes. Pressure signals carried by these waves affect the flow of water masses through a balance called the geostrophic relationship. We studied how ocean bottom pressure (OBP) and water flows in the North Atlantic Deep Water layer vary with the seasons. Our results show that these changes are driven by wind stress and are strongly affected by underwater features like ridges and valleys. Importantly, we found that seasonal changes are most noticeable in areas with pronounced seafloor features. While past studies have mostly focused on deep‐water flow along the western boundary, our research highlights the need to look at other regions to fully understand how deep ocean currents change with the seasons and how this impacts the Atlantic's large‐scale circulation system, known as the Atlantic Meridional Overturning Circulation (AMOC). Key Points Seasonal variability of pB in the North Atlantic is strongly influenced by topography, affecting both spatial patterns and magnitudes Interior pathways like Mid‐Atlantic Ridge are important for the southward transport of North Atlantic Deep Water (NADW) on the seasonal time scale NADW transport varies most profoundly along continental slopes, mid‐ocean ridges, and around seamounts

The Luzon Strait Deep Overflow (LZDO) transports deep‐water masses from the Pacific Ocean (upstream) to the South China Sea (SCS, downstream), playing a vital role in shaping the hydrographic and biogeochemical structure and regulating abyssal circulation within the SCS. Recent studies suggest that the seasonal variability of LZDO transport is primarily wind‐driven; however, the specific mechanisms and key wind‐forcing areas remain unclear. In this study, we use numerical model experiments to demonstrate that the seasonal variability of the LZDO is driven by wind stress both within the downstream SCS and upstream Pacific Ocean. This finding contrasts with previous views that considered the LZDO hydraulically controlled at the Luzon Strait sill and thus influenced solely by the upstream Pacific Ocean forcing. Additionally, we identify that the LZDO is particularly sensitive to wind forcing in specific North Pacific regions where geostrophic contours connect to the Luzon Strait due to topographic effects. Plain Language Summary Oceanic processes like ocean currents and the mixing of water in the South China Sea (SCS) are heavily influenced by exchange flows with nearby seas. The Luzon Strait, the only deep channel connecting the SCS with the Pacific Ocean, allows deep water to flow into or out of the SCS. This movement of deep water, known as the Luzon Strait Deep Overflow (LZDO), plays an important role in how the ocean circulates. However, the mechanisms driving the LZDO and its variability remain poorly understood, with most previous studies focusing on local processes around the Luzon Strait, such as Pacific‐SCS pressure differences. These pressure anomalies travel as waves, and their pathways are strongly influenced by the underlying topography due to the rules governing wave propagation. This study investigates both upstream and downstream wind forcings that contribute to the seasonal variability of the LZDO transport, revealing for the first time that wind‐stress forcing within the SCS plays a major role in modulating the LZDO's seasonal variation. Additionally, we identify the subpolar region in the upstream Pacific Ocean, which is the region with latitudes roughly around 40°N to 60°N, as a critical area affecting the LZDO's variability. Key Points Wind‐stress forcing in the downstream South China Sea is significant in regulating the seasonal variability of LZDO transport The subpolar area is the key region where the wind‐stress forcing is most effective in the upstream Pacific Ocean

The South China Sea (SCS) is a semi‐enclosed marginal sea linked to the broader oceans via various geographically constrained channels. Beneath the main thermocline depth, Luzon Strait is the only conduit for water‐mass exchanges. Observations indicate a substantial seasonal variability in the inflow transport of deep water from the Pacific Ocean. This study aims to identify and examine key drivers for such seasonal changes. It is found that seasonal variability of the deep‐water transport into the SCS is primarily driven by surface wind stress. An imbalance in wind‐driven exchanges of surface water between the SCS and external seas demands compensational transports in subsurface layers so that the net volume transport into the SCS is conserved, resulting in seasonal variations in deep‐water overflow. Changes in Karimata Strait exert a particularly influential impact on deep‐water inflow, likely due to its unique position as the sole connecting channel across the Equator. Plain Language Summary Observations show that the deep‐water inflow into the South China Sea (SCS) varies significantly with seasons. In this study, how wind stress influences this variability is examined. Using a 3‐layer model, we have identified that wind stress forces convergence and divergence of SCS upper‐layer water masses through straits lateral exchanges with adjacent seas. Such changes must be accommodated by adjustment of deep‐water inflow transport through Luzon Strait. Through this linkage, the wind stress inside the SCS strongly influences the seasonality of deep‐water inflow transport. Key Points Seasonal variability of the deep‐water transport into the South China Sea (SCS) is primarily driven by surface wind stress Convergence and divergence of wind‐driven transport into the SCS in the upper layer is compensated by transports in subsurface layers Transport variability through Karimata Strait has the most significant impact on deep‐water overflow variability

We present an observational study of the formation and disappearance of a funnel prominence. Before the funnel prominence formed, cool materials from the top of a preexisting polar crown prominence flowed along saddle-shaped coronal loops to their base, forming a smaller prominence. Meanwhile, the saddle-shaped coronal loops gradually rose, and U-shaped coronal loops, termed prominence horns, began to appear along with a coronal cavity. Afterward, a cool column emerged from the chromosphere, rose vertically into the corona, and then moved laterally to be transported into the U-shaped coronal loops. The formed prominence slid into the chromosphere, while the U-shaped coronal loops and the coronal cavity became more pronounced. As cool materials accumulated at the base of the U-shaped coronal loops, these loops underwent a significant descent and a V-shaped structure appeared at the base of the cool materials, indicating that the U-shaped coronal loops may be dragged down to sag. Subsequently, cool materials from the V-shaped structure continued to flow almost vertically toward the chromosphere, forming the funnel prominence. The vertical downflows might be produced by magnetic reconnection within or between the sagging field lines. Due to persistent vertical downflows, the U-shaped coronal loops were lifted up and prominence materials followed along inclined coronal loops toward the chromosphere, causing the funnel prominence to disappear. Our observations suggest that chromospheric plasma transported into a coronal cavity and then drained out via vertical downflows can form a funnel prominence.