Datasets of ionospheric parameters provided by SCINDA GNSS receiver from Lisbon airport area

Here we present datasets provided by a SCINDA GNSS receiver installed in Lisbon airport area from November of 2014 to July of 2019. The installed equipment is a NovAtel EURO4 with a JAVAD Choke-Ring antenna. The data are in the archived format and include the general messages on quality of records (*.msg), random number generator files (*.rng), raw observables as the signal-to-noise (S/N) ratios, pseudoranges and phases (*.obs), receiver position information (*.psn), ionosphere scintillations monitor (*.ism) and ionospheric parameters: total electron content, TEC, rate of change of TEC, ROTI, and the scintillation index S4 (*.scn). The presented data cover the full 2015 year. The raw data are of 1-minute resolution and available for each of receiver-satellite pairs. The processing and the analysis of the ionosphere scintillation datasets can be done using a dedicated "SCINDA-Iono" toolbox for MATLAB developed by T. Barlyaeva (2019) and available online via MathWorks File Exchange system. The toolbox allows to calculate 1-hour means for ionospheric parameters both for each of available receiver-satellite pairs and averaged over all available satellites during the analyzed hour. Here we present also the processed data for the following months in 2015: March, June, October, and December. The months were selected as containing most significant geomagnetic events of 2015. The 1-hour means for other months can be obtained from the raw data using, e.g. the aforementioned toolbox. The provided datasets can be of interest for the GNSS and ionosphere scientific communities

Datasets of ionospheric parameters provided by SCINDA GNSS receiver from Lisbon airport area

Here we present datasets provided by a SCINDA GNSS receiver installed in Lisbon airport area from November of 2014 to July of 2019. The installed equipment is a NovAtel EURO4 with a JAVAD Choke-Ring antenna. The data are in the archived format and include the general messages on quality of records (*.msg), random number generator files (*.rng), raw observables as the signal-to-noise (S/N) ratios, pseudoranges and phases (*.obs), receiver position information (*.psn), ionosphere scintillations monitor (*.ism) and ionospheric parameters: total electron content, TEC, rate of change of TEC, ROTI, and the scintillation index S4 (*.scn). The presented data cover the full 2015 year. The raw data are of 1-minute resolution and available for each of receiver-satellite pairs. The processing and the analysis of the ionosphere scintillation datasets can be done using a dedicated "SCINDA-Iono" toolbox for MATLAB developed by T. Barlyaeva (2019) and available online via MathWorks File Exchange system. The toolbox allows to calculate 1-hour means for ionospheric parameters both for each of available receiver-satellite pairs and averaged over all available satellites during the analyzed hour. Here we present also the processed data for the following months in 2015: March, June, October, and December. The months were selected as containing most significant geomagnetic events of 2015. The 1-hour means for other months can be obtained from the raw data using, e.g. the aforementioned toolbox. The provided datasets can be of interest for the GNSS and ionosphere scientific communities.THIS DATASET IS ARCHIVED AT DANS/EASY, BUT NOT ACCESSIBLE HERE. TO VIEW A LIST OF FILES AND ACCESS THE FILES IN THIS DATASET CLICK ON THE DOI-LINK ABOV

Mid-Term Quasi-Periodicities and Solar Cycle Variation of the White-Light Corona from 18.5 Years (1996.0-2014.5) of LASCO Observations

International audienceWe report on the analysis of the temporal evolution of the solar corona based on 18.5 years (1996.0 -aEuro parts per thousand 2014.5) of white-light observations with the SOHO/LASCO-C2 coronagraph. This evolution is quantified by generating spatially integrated values of the K-corona radiance, first globally, then in latitudinal sectors. The analysis considers time series of monthly values and 13-month running means of the radiance as well as several indices and proxies of solar activity. We study correlation, wavelet time-frequency spectra, and cross-coherence and phase spectra between these quantities. Our results give a detailed insight on how the corona responds to solar activity over timescales ranging from mid-term quasi-periodicities (also known as quasi-biennial oscillations or QBOs) to the long-term 11 year solar cycle. The amplitude of the variation between successive solar maxima and minima (modulation factor) very much depends upon the strength of the cycle and upon the heliographic latitude. An asymmetry is observed during the ascending phase of Solar Cycle 24, prominently in the royal and polar sectors, with north leading. Most prominent QBOs are a quasi-annual period during the maximum phase of Solar Cycle 23 and a shorter period, seven to eight months, in the ascending and maximum phases of Solar Cycle 24. They share the same properties as the solar QBOs: variable periodicity, intermittency, asymmetric development in the northern and southern solar hemispheres, and largest amplitudes during the maximum phase of solar cycles. The strongest correlation of the temporal variations of the coronal radiance - and consequently the coronal electron density - is found with the total magnetic flux. Considering that the morphology of the solar corona is also directly controlled by the topology of the magnetic field, this correlation reinforces the view that they are intimately connected, including their variability at all timescales

Comparing the solar minima of cycles 22/23 and 23/24: The view from LASCO white light coronal images

International audienceThe Large Angle and Spectrometric Coronagraph LASCO-C2 aboard SOHO has now completed 17 years (1996-2012) of quasi-continuous white-light imaging of the corona from 2.2 to 6.5 solar radii, thus allowing an unprecedented view of its evolution over a solar cycle and a half including the minima of solar cycles 22/23 and 23/24. The corrected and calibrated polarization sequences produce images of the radiance (B), the polarized radiance (pB), and the electron density N-e of the K corona, and, in turn, of their synoptic maps. Their temporal variations are quantified by integration first globally, then in the north and south hemispheres, and finally, in sectors of 30 degrees latitudinal extent centered along the equatorial and polar directions. The global radiance of the K corona follows well the solar activity as described by the sunspot number and the radio flux and was 24% fainter during the minimum of solar cycle 23/24 than during that of cycle 22/23. However, the two hemispheres experienced different reductions, 17% for the north one and 29% for the south one. The equatorial sector suffered a drastic reduction of 44%, in remarkable agreement with the in situ measurements of Wind and ACE at 1 AU, whereas the north and south polar sectors did not experience much variation. Cycle 23 is estimated to have lasted 12 years and 3 months. Maximum conditions have been reached in the northern region, whereas the southern region is still lagging. Finally, the rate of coronal mass ejections follows well the solar activity

Link of volcanic activity and climate change in Altai studied in the ice core from Belukha Mountain

In the present research we discuss a role of volcanic activity in Altai thermal regime. Here we analyses the sulfate and temperature data reconstructed from the natural paleoarchive – ice core from the Belukha Mountain saddle. Sulfate ice-core reconstructions can serve as volcanic markers. The both – sulfate and temperature reconstructions – are for the last 750 years. As the characteristic of volcanic activity we consider Volcanic Explosivity Index (VEI), Dust Veil Index (DVI) and Ice core volcanic index (IVI). The analysis was done using wavelet analysis and analysis of wavelet cross coherence and phase. As the result, we conclude that observed increases in the values of the indexes VEI, DVI, IVI basically correspond to decreases of temperature and increases of sulfate concentrations. This confirms the dependence of changes in the thermal regime of the Altai from volcanic activity. But in the 1750–1850 years period there is a delay of the changes in temperature with respect to the changes in volcanic activity. We suggest that it can be due to the superposition of the influence of solar and volcanic activity on changes in the thermal regime of Altai

Rotation of the Earth, solar activity and cosmic ray intensity

International audienceWe analyse phase lags between the 11-year variations of three records: the semi-annual oscillation of the length of day (LOD), the solar activity (SA) and the cosmic ray intensity (CRI). The analysis was done for solar cycles 20-23. Observed relationships between LOD, CRI and SA are discussed separately for even and odd solar cycles. Phase lags were calculated using different methods (comparison of maximal points of cycles, maximal correlation coefficient, line of synchronization of cross-recurrence plots). We have found different phase lags between SA and CRI for even and odd solar cycles, confirming previous studies. The evolution of phase lags between SA and LOD as well as between CRI and LOD shows a positive trend with additional variations of phase lag values. For solar cycle 20, phase lags between SA and CRI, between SA and LOD, and between CRI and LOD were found to be negative. Overall, our study suggests that, if anything, the length of day could be influenced by solar irradiance rather than by cosmic rays

Coronal Mass Ejections over Solar Cycles 23 and 24

International audienceWe present a statistical analysis of solar coronal mass ejections (CMEs) based on 23 years of quasi-continuous observations with the LASCO coronagraph, thus covering two complete Solar Cycles (23 and 24). We make use of five catalogs, one manual (CDAW) and four automated (ARTEMIS, CACTus, SEEDS, and CORIMP), to characterize the temporal evolutions and distributions of their properties: occurrence and mass rates, waiting times, periodicities, angular width, latitude, speed, acceleration and kinetic energy. Our analysis points to inevitable discrepancies between catalogs due to the complex nature of CMEs and to the different techniques implemented to detect them, but also to large areas of convergence that are critically important to ascertain the reliability of the results. The temporal variations of these properties are compared to four indices/proxies of solar activity: the radio flux at 10.7 cm (F10.7), the international sunspot number (SSN), the sunspot area (SSA), and the total magnetic field (TMF), either globally or separately in the northern and southern hemispheres in the case of the last three. We investigate the association of CMEs with flares, erupting prominences, active regions and streamers. We find that the CME occurrence and mass rates globally track the indices/proxies of solar activity with no time lag, prominently the radio flux F10.7, but the linear relationships were different during the two solar cycles, implying that the CME rates were relatively larger during SC 24 than during SC 23. However, there exists a pronounced divergence of the CME rates in the northern hemisphere during SC 24 as these rates were substantially larger than predicted by the temporal variation of the sunspot number. The distribution of kinetic energy follows a log-normal law and that of angular width follows an exponential law implying that they are random and independent. The distribution of waiting time (WTD) has a long power-law tail extending from 3 to 100 hr with a power-law index which varies with the solar cycle, thus reflecting the temporal variability of the process of CME formation. There is very limited evidence for periodicities in the occurrence and mass rates of CMEs, a striking feature being the dichotomy between the two hemispheres. Rather weak correlations are present among the various CME parameters and particularly none between speed and acceleration. The association of CMEs with flares and erupting prominences involves only a few percents of the overall population of CMEs but the associated CMEs have distinctly larger mass, speed, kinetic energy and angular width. A more pronounced association is found with active regions but the overwhelming one is with streamers further confirmed by the similarity between the heliolatitudinal distribution of CMEs and that of the electron density reconstructed from time-dependent tomographic inversion. We find no evidence of bimodality in the distributions of physical parameters that would support the existence of two classes, particularly that based on speed and acceleration, the distributions thus favoring a continuum of properties. There exists an excess of narrows CMEs which however does not define a special class. These narrow CMEs are likely associated with the ubiquitous mini-filaments eruptions and with mini flux ropes originating from small magnetic bipoles, the disruption mechanisms being similar to those launching larger CMEs. This supports the concept that CMEs at large arise from closed-field coronal regions at both large and small scales

Связь вулканической активности и климатических изменений на Алтае по данным исследования ледникового керна горы Белуха

In the present research we discuss a role of volcanic activity in Altai thermal regime. Here we analyses the sulfate and temperature data reconstructed from the natural paleoarchive – ice core from the Belukha Mountain saddle. Sulfate ice-core reconstructions can serve as volcanic markers. The both – sulfate and temperature reconstructions – are for the last 750 years. As the characteristic of volcanic activity we consider Volcanic Explosivity Index (VEI), Dust Veil Index (DVI) and Ice core volcanic index (IVI). The analysis was done using wavelet analysis and analysis of wavelet cross coherence and phase. As the result, we conclude that observed increases in the values of the indexes VEI, DVI, IVI basically correspond to decreases of temperature and increases of sulfate concentrations. This confirms the dependence of changes in the thermal regime of the Altai from volcanic activity. But in the 1750–1850 years period there is a delay of the changes in temperature with respect to the changes in volcanic activity. We suggest that it can be due to the superposition of the influence of solar and volcanic activity on changes in the thermal regime of Altai.Впервые с помощью вейвлет-анализа и анализа вейвлет-кросскогерентности и фаз проанализирована связь климатических изменений на Алтае, реконструированных по данным высокогорного ледникового керна, взятого с седловины горы Белуха, и вулканической активности, описанной индексами VEI, DVI и IVI, за последние 750 лет. Полученные фазовые соотношения изменений концентраций сульфатов в керне и вулканических индексов, а также противофазные низкочастотные статистически значимые сигналы между индексами вулканической активности и температурой воздуха позволяют говорить о зависимости изменений термического режима на Алтае от вулканической активности. При этом в малый ледниковый период отмечается запаздывание климатических изменений относительно вулканической деятельности, что может быть связано с наложением влияния солнечной активности на изменения термического режима