Introduction to Venus Express

What is/are Venus Express?

Venus Express - We used the high-resolution iSHELL spectrometer located at the NASA IRTF to record thermal night-side spectra, which we fitted using an updated forward radiative transfer model that was previously employed to process SpeX/IRTF and VIRTIS-H/Venus Express spectra. ^[1] Guided by the remarkably consistent morphological appearance of this feature, we have identified at least one previous instance of it in the Venus Express Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) data. ^[2] In 2010 the ESA Venus Express Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) instrument first observed 1 μm emissivity anomalies over the top and eastern flank of Idunn Mons (46° S; 146° W), a 200 km wide volcano located in Imdr Regio, a volcano-dominated large volcanic rise of Venus. ^[3] This circumstance led to a long standstill for further space programs to Venus after the first space-based explorations of this planet in the 1970s through the mid-1990s, which was not broken until the launch of ESA's Venus Express (VEX) mission in 2005. ^[4] These neurons were spatially clustered, exhibited intermittently repeated dVenus expression, and often continued to express Arc-dVenus for approximately two weeks. ^[5] The Venus Express radio science experiment VeRa provided more than 900 neutral atmospheric profiles between the years 2006 and 2014. ^[6] Experiments involving the radio sounding of solar plasma with signals from the Venus Express and Mars Express spacecraft, which were carried out from October 6 to December 6, 2006, provided data on frequency fluctuations of the radio signals for the western and eastern coronal limbs. ^[7] Based on the Venus Express data, 115 quasi-parallel ( $$Q_{\parallel }$$ Q ‖ ) bow shock crossings and 303 quasi-perpendicular ( $$Q_{ \bot }$$ Q ⊥ ) bow shock crossings are selected. ^[8] In hypothalamic organotypic cultures from the AVP-Venus mice, Venus-labeled AVP neurons in the supraoptic and paraventricular nuclei survived for 1 month, and Venus expression was upregulated by forskolin. ^[9] The selected CME eruption occurred on the 6th of January 2013 and was encountered by two spacecraft, Venus Express and STEREO--A, which were radially aligned at the time of the CME passage. ^[10] Latitudinal variations of mode mixtures as interpreted by the M3L coordinates were compared with those in the Venus Express observation-based studies. ^[11] We will present here several comparisons of the upper atmosphere of Venus between our model results and a selection of aerobraking data from different missions such as Venus Express, Pioneer Venus and Magellan. ^[12] Here we study the well-structured Venusian IMB with a sudden magnetic field rotation and a sharp magnetosheath plasma decrease using Venus Express observations. ^[13] We focus on an eruption from 6 January 2013 encountered by two radially aligned spacecraft, Venus Express and STEREO-A. ^[14] We present the detection and characterisation of mesoscale waves on the lower clouds of Venus using images from the Visible Infrared Thermal Imaging Spectrometer (VIRTIS-M) onboard the European Venus Express space mission and from the 2 μm camera (IR2) instrument onboard the Japanese space mission Akatsuki. ^[15] We focus on the validation of the model built from a collection of data mostly from Venus Express (2006-2014) experiments and coordinated ground-based telescope campaigns, in the upper mesosphere/lower thermosphere of Venus (80-150 km). ^[16] The measurements from the Venus Express spacecraft are analyzed for the basic properties of fast forward interplanetary shocks at Venus’s orbit (∼0. ^[17] Our results are consistent with the observation of Venus Express space probe. ^[18] Following the co-injection of the piwil1-Venus expression vector and the Tol2 transposase mRNA into fertilized eggs, presumptive transgenic fish were reared. ^[19] We present a study of the SOIR/Venus Express CO2 and CO profiles in order to constrain the eddy diffusion profile in the Venus mesosphere (80 to 130 km of altitude). ^[20] We test our automatic procedure by applying it to the magnetic field data measured by the FGM onboard Venus Express. ^[21] From the early flyby transit of the Mariner 5 spacecraft to the later orbit crossings of the Venera 10, the Pioneer Venus and more recently the Venus Express there has been accumulated evidence of the presence of that transition by the flanks of the Venus wake. ^[22] 5-year dataset (May 2006 to December 2014) of the Ion Mass Analyzer and the magnetometer aboard Venus Express. ^[23] We investigate the heavy ion density and velocity in the Venusian upper ionosphere near the North Pole, using the Ion Mass Analyzer, a part of the Analyzer of Space Plasmas and Energetic Atoms 4, together with the magnetic field instruments on Venus Express. ^[24] Our result is consistent with earlier estimates (but with smaller uncertainties), including those based on offsets between Venus Express infrared mapping data and Magellan topography that suggest a mean LOD of 243. ^[25] More concretely, the Venus Monitoring Camera (VMC) onboard Venus Express orbiter provided the largest and the longest so far set of ultraviolet (UV), visible and near-IR images for investigation of the atmospheric circulation. ^[26] Here we validate the current version of the Institut Pierre Simon Laplace (IPSL) Venus GCM, by means of a comparison between the modelled temperature field and that obtained from data by the Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) and the Venus Express Radio Science Experiment (VeRa) onboard Venus Express. ^[27] On 2011 November 5, Venus Express observed the impact of an extremely strong interplanetary coronal mass ejection (ICME) on Venus. ^[28] In adulthood, however, there was a significant female predominance in the number of Venus expressing neurons in two subnuclei of the dorsolateral BNST, i. ^[29] Flow cytometry was used to assess Venus expression in different cell populations. ^[30] Using data from the MESSENGER, Venus Express and ACE spacecraft, we analyze with the superposed epoch technique the profiles of ICME substructures, namely the sheath and the magnetic ejecta. ^[31] Finally, there is a good agreement between the TEXES results and those obtained in the UV range (SPICAV/Venus Express and UVI/Akatsuki) at a slightly higher altitude. ^[32] Winds derived by a digital tracking technique from UV (365 nm) images captured by the Venus Monitoring Camera onboard the Venus Express spacecraft from 2006 through 2013 were used to study the atmospheric circulation at cloud top level (70±2 km). ^[33] Moreover, ovariectomy resulted in the absence of OXTR-Venus expression in the AVPV, whereas estrogen replacement therapy restored OXTR-Venus expression. ^[34] In this work, we present a comprehensive catalog of 47 CMEs measured in situ measurements by two or more radially aligned spacecraft (MESSENGER, Venus Express, STEREO or Wind/ACE). ^[35] 1-μm emissivity was derived using Venus Monitoring Camera (VMC) measurements on board of Venus Express (VEx). ^[36] We conducted a test with ESA's Venus Express (VEX), to evaluate the performance of the PRIDE technique for this particular application. ^[37] The atmospheric composition has been studied to some extent with the Pioneer Venus Orbiter mission and the more recent Venus Express, however, the concentration of many species and their isotopic ratios are not yet known with satisfying accuracy. ^[38] The application of PRIDE for atmospheric studies has been demonstrated by observing ESA's Venus Express (VEX) during multiple Venus occultation events (Bocanegra-Bahamon et al. ^[39]

Onboard Venus Express

We test our automatic procedure by applying it to the magnetic field data measured by the FGM onboard Venus Express. ^[1] More concretely, the Venus Monitoring Camera (VMC) onboard Venus Express orbiter provided the largest and the longest so far set of ultraviolet (UV), visible and near-IR images for investigation of the atmospheric circulation. ^[2]

venus express radio

The Venus Express radio science experiment VeRa provided more than 900 neutral atmospheric profiles between the years 2006 and 2014. ^[1] Here we validate the current version of the Institut Pierre Simon Laplace (IPSL) Venus GCM, by means of a comparison between the modelled temperature field and that obtained from data by the Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) and the Venus Express Radio Science Experiment (VeRa) onboard Venus Express. ^[2]

venus express spacecraft

The measurements from the Venus Express spacecraft are analyzed for the basic properties of fast forward interplanetary shocks at Venus’s orbit (∼0. ^[1] Winds derived by a digital tracking technique from UV (365 nm) images captured by the Venus Monitoring Camera onboard the Venus Express spacecraft from 2006 through 2013 were used to study the atmospheric circulation at cloud top level (70±2 km). ^[2]

venus express visible

Guided by the remarkably consistent morphological appearance of this feature, we have identified at least one previous instance of it in the Venus Express Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) data. ^[1] In 2010 the ESA Venus Express Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) instrument first observed 1 μm emissivity anomalies over the top and eastern flank of Idunn Mons (46° S; 146° W), a 200 km wide volcano located in Imdr Regio, a volcano-dominated large volcanic rise of Venus. ^[2]

venus express observation

Latitudinal variations of mode mixtures as interpreted by the M3L coordinates were compared with those in the Venus Express observation-based studies. ^[1] Here we study the well-structured Venusian IMB with a sudden magnetic field rotation and a sharp magnetosheath plasma decrease using Venus Express observations. ^[2]

venus express space

We present the detection and characterisation of mesoscale waves on the lower clouds of Venus using images from the Visible Infrared Thermal Imaging Spectrometer (VIRTIS-M) onboard the European Venus Express space mission and from the 2 μm camera (IR2) instrument onboard the Japanese space mission Akatsuki. ^[1] Our results are consistent with the observation of Venus Express space probe. ^[2]