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Quantifying how tides evolve with coupling between future sea level rise (SLR) and different coastline configurations is imperative for proposing appropriate coastal defense strategies. By using numerical models, we investigated tidal changes and determined a realistic trend of SLR on the Jiangsu coastal area and adjacent sea on the Yellow Sea shelf. A notable decrease in tidal range occurs in the northern shelf, and the tide increases mainly in the southern shelf. Tidal changes are of both signs, while the increase in sea level is unidirectional. Thus, the SLR effect on tide is not additive in all locations. We also explored the nonlinearity and spatial similarity in tidal range in response to the SLR considering uniform SLR scenarios with multiple levels and allowing inundation of the natural coastline. The patterns of change in tide evolution on the study domain remain linear until the SLR exceeds 2.0 m. Simulations and comparisons are further conducted between the responses of hardened and natural shoreline configurations to SLR. Hardened shoreline introduces both local and remote spatial variability in tidal responses. On the regional scale, SLR induces a shift in the tidal system in the offshore region, which controls the net energy flux into the embayment upon the coast. On the local scale, tidal dynamics are mainly a competition between net energy flux and tidal dissipation and are plausibly influenced by tidal reflection, which depends on whether a basin is tidally reflective. China has experienced rapid economic growth and irreversible pressures from sea level rise (SLR) in the eastern coastal region. To provide future coastal defense strategies, we conduct multiple experiments to simulate how tides evolve with future SLR scenarios as well as how tides respond to different coastline configurations. We found that the future SLR can adjust the entire tidal system and control how much tidal energy flows into the local area from the deep ocean. Whether to build up or maintain a seawall for coastal defense depends on local conditions. By preserving the natural coast and removing the impermeable seawall from the radial sand ridges of China, tidal waves become more progressive on the shoals. Tidal change remains linear under a 2.0‐m sea level rise within which a large spatial similarity was achieved on the Yellow Sea shelfDisplacement in the amphidromic point on the northern Yellow Sea shelf dominates the tidal range evolution for the Jiangsu coastal areaThe seawall of Jiangsu with SLR enlarges the tidal range where the tide is reflective but functions opposite where the tide is parallel to the coast

In this paper, the CESE‐HLL three‐dimensional magnetohydrodynamic solar wind model is first modified to be able to work in a corona‐heliosphere integrated approach and then used to simulate the evolution of solar wind from the solar surface to the Earth's orbit during year 2008. Here high‐cadence photospheric magnetic field data are used to drive the model at the solar surface via the projected normal characteristic boundary equations. The simulated results are analyzed and quantitatively evaluated by comparing the simulated results with solar and interplanetary observations. The analyses demonstrate that our model reproduces the main pattern and the evolutionary feature of large‐scale coronal structures. The simulated results show that the height of the pseudostreamer X point is positively correlated with the distance of the coronal holes connected by the pseudostreamer. During year 2008, the helmet streamer belt is found to have a net southward displacement from the equator while the pseudostreamer belts are biased to the Northern Hemisphere. Both helmet streamer belt and pseudostreamer belts exhibit a general trend of becoming more concentrated along the equator throughout 2008. The evaluation of the simulated results at the L1 point shows that the general structures can be generated by the model, and that speed is the best among the solar wind parameters reproduced. However, the temperature of the fast solar wind and the magnitude of the interplanetary magnetic field are underestimated. The success rate of prediction and arrival time error are also calculated for magnetic field polarity reversals and stream interaction regions. Magnetic field data‐driven simulation of the ambient solar wind is carried out for the whole of year 2008Analysis of the solar wind evolution is focused on helmet streamer and pseudostreamer global structureSimulation results are evaluated quantitatively by comparison with in situ measurements

The global distributions of photospheric magnetic field are routinely provided by synoptic maps, which often serve as fundamental observational input for coronal and heliospheric models. In this paper, we compare synoptic maps and PFSS‐derived magnetic field results obtained during 2017/12/06–2018/12/06, a period at the declining phase of solar cycle 24. We use four kinds of synoptic maps, the Helioseismic and Magnetic Imager (HMI) maps, the Air Force Data Assimilative Photospheric Flux Transport (ADAPT) maps, the Global Oscillation Network Group (GONG) maps with their zero‐point uncertainty corrected (GONGz maps) or uncorrected (GONGb maps). Qualitatively similarity among the four maps are found in the low‐latitude region, but the polar fields have notable differences. While the polar fields of HMI, ADAPT and GONGz maps are unipolar and relative stable in large scale, those of the GONGb maps are variable. The PFSS results of HMI, ADAPT, and GONGz compare reasonably with coronal remote observations and near‐Earth in situ data, and the HMI maps perform slightly better. There is generally no significant difference among results of the 12 ADAPT ensemble maps, but exceptions are also found. The PFSS results of GONGb maps deviate from observation significantly. The deviations are attributed to the problematic polar field, and the source of the problem may be the zero‐point uncertainty of the magnetograms. As GONGb maps perform well in the declining phase of solar cycle 23, results in this study highlight the importance of continuous assessment of synoptic map data quality. Photospheric synoptic maps and PFSS solutions obtained during 2017/12/06–2018/12/06 are comparedThe zero‐point uncertainty of the magnetograms may affect the high‐latitude data and bring in problematic polar fields for the synoptic mapsIt is necessary to continuously assess data quality of synoptic maps Photospheric synoptic maps and PFSS solutions obtained during 2017/12/06–2018/12/06 are compared The zero‐point uncertainty of the magnetograms may affect the high‐latitude data and bring in problematic polar fields for the synoptic maps It is necessary to continuously assess data quality of synoptic maps