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A striking change in the external stakeholders’ engagement due to unexpected scenarios as a result of COVID-19 pandemic has hurled the medical affairs (MA) function into innovative strategies of scientific engagements and patient-centric activities. Expansion of MA functions including rising regulatory and compliance inspections, an increased patient centricity and more requirements for RWE, have created the importance of medical affairs not just being the support function but as a trusted strategic pillar in the pharmaceutical and healthcare industry. There is certainly a silver lining due to strong digital transformation within these adverse times. The present review is focused on digital transformation for dissemination of medical information and its advantages over traditional ways. In today’s pandemic era HCPs have embraced the idea of virtual CMEs and digital storytelling which has necessitated the MA function to become more agile, adapted and look for collaborations. Both the exponential and radical improvements are required to strengthen this transition, in the new normal of a post-COVID era. The digital innovation in three key vitals viz. HCP engagement, external partnerships and data generation will allow MA to become future fit as a strategic leadership function. Moreover, the recommendations from executive committees of renowned international societies such as APPA, IFAPP, MAPS and MSLS, who have contributed for MA function to create their own standard operating procedures (SOPs), policies which are relevant for industry, are also discussed. Keywords: COVID-19, digital transformation, massive open online courses, medical affairs, omni-channel; real- world evidence

The aim of the study was to present a case of primary abdominal pregnancy, a rare entity and highlighting the diagnostic dilemma and importance of surgical management. Primigravida with an amenorrhea of 35 days presented to the casualty with acute abdomen, with faintly positive UPT test and USG pelvis was suggestive of ill-defined hypoechoeic mass lesion in right sided adnexal region abutting right ovary. Intra-operatively, blood clots with products of conception were found adherent to anterior layer of right broad ligament. Uterus, both fallopian tubes and both ovaries found intact with normal morphology. On histopathology, no chorionic villi was found inside the lumen of the fallopian tube. Presence of occasional ghost chorionic villi embedded in blood clots, scattered cytotrophoblast and syncytiotrophoblasts also seen in the sample obtained from the anterior leaf of broad ligament. Primary abdominal pregnancy is not only rare but the diagnosis is also a challenge. It can be diagnosed conclusively after laparotomy. There are no symptoms which are pathognomonic for abdominal pregnancy. The symptoms are akin to other types of ectopic pregnancy, so a high index of suspicion is highly necessary for diagnosis. The keys to management are an early diagnosis and prompt surgery.

The Emirates Mars Ultraviolet Spectrometer (EMUS) onboard the Emirates Mars Mission spacecraft, which observes ultraviolet emission between approximately 100 and 170 nm, has observed multiple instances of nightside aurora at Mars. Variations in the auroral brightness and morphology have been observed to change on timescales of tens of minutes. The brightest aurorae are typically seen following space weather events, i.e., coronal mass ejection and stream interaction region impacts. The InSight Fluxgate Magnetometer (IFG) on the Interior Explorations using Seismic Investigations, Geodesy and Heat Transport (InSight) lander measured the magnetic field at the surface of Mars. IFG has measured variations in the nightside surface magnetic field, presumably due to variations in ionospheric and magnetospheric currents. Periodic and aperiodic variations in the surface field have been observed, including with timescales of a few minutes to tens of minutes. The magnitude of the fluctuations is often larger following space weather events. We examine the connection between the presence of aurora as observed by EMUS and surface magnetic field fluctuations as measured by IFG. Coincident EMUS and IFG observations show enhanced surface magnetic field fluctuations during times when aurorae were present. Additionally, the timescale of fluctuations in the auroral brightness are similar to the timescale of surface magnetic field fluctuations for non-coincident observations. These results suggest that IFG measured the surface magnetic field effect of time varying ionospheric auroral currents.

The Emirates Mars Mission (EMM) Hope probe launched on 20 Jul 2020 and entered Mars orbit on 9 Feb 2021, carrying a payload of 3 complementary instruments to characterize the global atmosphere across the full range of altitudes (surface to exosphere) at diurnal and seasonal timescales. The unique, high-altitude orbit of the Hope probe (19,970 km periapse, 42,650 km apoapse altitude, 25 deg inclination, 54.5-hour period) that enables its synoptic view of the red planet also brings the spacecraft across the orbit of Mars’ outermost moon, Deimos. The Hope trajectory was slightly modified by two maneuvers in Aug 2022 and Jan 2023 that will allow the surface of Deimos to be observed in a series of flybys in Feb-Mar 2023. Here we present preliminary results from the Emirates Mars Ultraviolet Spectrometer (EMUS), an imaging spectrograph with a wavelength range of 100-170 nm and a field of view of 10.75 x 0.18 deg (using the high-resolution slit position). We will derive the absolute reflectance of the surface, search for any compositionally distinct spectral features (e.g. carbon, polycyclic aromatic hydrocarbons, water ice), and examine any spatial heterogeneity across the surface.

Atomic hydrogen and oxygen are the dominant species in the Martian exosphere. Atomic hydrogen is essentially produced from the dissociation of H2O, whereas, hot oxygen atoms are populated by non-thermal processes such as the dissociative recombination of O2+ with electrons in the Martian ionosphere. The study of these species helps to understand the evolution of the Martian atmosphere and more specifically the history of water on Mars. The Emirates Mars Ultraviolet Spectrometer (EMUS), one of the primary instruments onboard the Emirates Mars Mission (EMM), has been observing atomic hydrogen and oxygen in the Martian exosphere over the Mars Year 36. We present the analysis of the cross-exospheric observations by the EMUS for hydrogen Lyman series and oxygen 130.4 nm emissions and their seasonal variability. The EMUS cross-exospheric observations cover the tangent altitude starting from 130 km to more than 35,000 km above the disk (see Fig. 1), with most of the observations below 25,000 km. The observations show that when Mars moved from perihelion to aphelion, the hydrogen emission line intensities increase by an order of magnitude or more whereas, for oxygen, it is an increment by a factor of about 2 at larger altitudes. Based on these observations, we also discuss the retrieval of densities, temperature, and the estimation of escape fluxes of hydrogen and oxygen species by applying 3D hydrogen ballistic corona and 3D Monte Carlo particle transport models, respectively.Figure 1: The EMM-observed cross-exosphere emission intensity profiles of atomic hydrogen and oxygen during Mars Year 3

One of the primary objectives of the Emirates Mars Mission (EMM) is to study the seasonal variation of the upper atmosphere of Mars and associated changes in the escape of atmosphere to space. Here we present a preliminary analysis of the oxygen population in the inner exosphere (1.06-1.6 Martian radii) with nearly-contiguous sampling across all Martian seasons from early MY 36 to early MY 37. This oxygen is thought to be a non-thermal photochemically generated population driven by solar EUV, which can produce energetic atoms with sufficient velocity to escape Mars’ gravity. The observations are made by measuring the atomic oxygen emission at 130.4 nm using the Emirates Mars Ultraviolet Spectrometer (EMUS). We compare the brightness of the exospheric oxygen population with the thermospheric population ( < 1.06 Mars radii, or < 200 km) and find that the exosphere is much more responsive to seasonal variations in solar energy input. The seasonal variations cannot be explained by modulations in solar irradiance at 130.4 nm alone, and are consistent with the expectation that the extended oxygen exosphere at Mars is generated by a photochemical source.

The presence of a weak oxygen emission at 130.4-nm resulting from the O 3P-3S transition was first detected in limb observations of the Martian aurora with SPICAM/Mars Express (Soret et al., 2016). It is mostly excited by direct impact of energetic electrons on ground-based O(3P) atoms, but the 130.4-nm radiation is affected by multiple scattering and absorption by CO2. In April 2021, the Emirates Mars Ultraviolet Spectrometer (EMUS) instrument (Holsclaw et al., 2021) on board the HOPE Emirates orbiter started collecting spectral images in the 110-180 nm range with a much increased sensitivity. The OI 135.6-nm emission corresponding to the 3P-5S forbidden transition has also been observed (Jain et al., 2022). In addition, EMUS is taking images of the discrete and sinuous aurora at 130.4 nm. We present Monte Carlo model simulations of the production of the O 3S and 5S excited states for different initial electron energies and discuss possible seasonal variations. We solve the radiative transfer equation for the 130.4-nm triplet and show that the I(130.4 nm/I(135.6 nm) nadir intensity ratio is expected to widely vary with the initial electron energy. These variations result from two effects:The different shapes of the two emission cross sections since the optically thick 3P-3S resonance transition is permitted while 3P-5S is forbidden the radiation entrapment of the 130.4 nm triplet by atmospheric atomic oxygen coupled with absorption by CO2. We also discuss the sensitivity of the 130.4-nm nadir brightness to the energy distribution of the incoming auroral electrons. ReferencesJain, S. et al. (2022), poster presented at AGU fall meeting.Holsclaw, G. et al. (2021), Space Science Reviews, 217, 1-49.Lillis, R. J. et al. (2022), Geophysical Research Letters, 49, e2022GL099820.Soret, L. et al. (2016), Icarus, 264, 398-406.

The Emirates Mars Ultraviolet Spectrometer (EMUS) onboard the Emirates Mars Mission (EMM) observes the Martian dayglow at ultraviolet wavelengths (100-170 nm). EMUS disk observations show unexpected variations in atomic hydrogen, atomic oxygen, and carbon monoxide disk emissions. These variations display local time and hemispheric asymmetry and are observed in approximately 25% of the disk images. England et al. (2022; doi:10.1029/2022GL099611) suggested that the spatial structure, occurrence, and spectral characteristics of these variations are associated with changes in composition and photoelectron flux. Using a similar EMUS data set, Chaffin et al. (2022; doi:10.1029/2022GL099881) reported the first observations of neutral atmosphere auroral emission on the Martian dayside, which is not a new type of aurora but another observable form of proton aurora, and suggested that solar wind deposition is responsible for exciting the auroral emission. We further investigate these two potential drivers of the unexpected variations in EMUS disk observations using data from the Imaging Ultraviolet Spectrograph (IUVS), the Solar Wind Ion Analyzer (SWIA), the SupraThermal And Thermal Ion Composition (STATIC) instrument, and a magnetometer (MAG), all onboard NASA’s Mars Atmosphere and Volatile EvolutioN (MAVEN) mission. We use vertical profiles of densities and temperatures retrieved from limb scan observations by IUVS to identify signatures of dynamics that correlate with unexpected variations in EMUS disk observations. We use measurements from all of the instruments to categorize and characterize EMUS observations in order to determine how changes in composition and solar wind deposition produce unexpected variations in the Martian ultraviolet dayglow.

The surface of the planet Mars exhibits a record of dessiccation and oxidation, the legacy of significant water escape to space as hydrogen and oxygen. This H escape can be constrained using ultraviolet observations of the planet's upper atmosphere, where neutral atomic hydrogen scatters UV sunlight. In the time since its orbit insertion in early 2021, the Emirates Mars Ultraviolet Spectrometer (EMUS) on the Emirates Mars Mission (EMM) has been observing this hydrogen at 102.6 nm and 121.6 nm, H Lyman beta and Lyman alpha. Here we present H escape rates retrieved from these observations, obtained using a 3D radiative transfer model that simulates the brightness of both spectral lines, combining their information content to constrain the atmospheric state. In agreement with past results, we find that H escape peaks around Southern Summer solstice, after perihelion, exhibiting a more than 10x increase relative to Northern Summer conditions. Importantly, our retrievals extract information about both the hydrogen density and temperature, and do not require independent assumptions about the upper atmosphere temperature. We will discuss prospects for extending these retrievals beyond the current EMM dataset as well as implications for the long-term evolution of the Mars atmosphere.

The major scientific objective of the Emirates Mars Mission (EMM) is to explore the global atmospheric dynamics of the Martian atmosphere both in short term (diurnal) and long term (seasonal). The Emirates Mars Ultraviolet Spectrometer (EMUS) instrument on board the EMM makes two-dimensional images ( in extreme and far ultraviolet wavelengths: 90-170 nm) of the Martian disk and exosphere to characterize the neutral densities in the thermosphere and exosphere of Mars. In this paper, we will present the first results from the stellar occultation measurements made by the EMUS instruments in October 2022. These occultation observations were not part of the original science planning and were added as a bonus EMM science. A total of seven stellar occultations were performed during the two EMM orbits spanning between 24 to 27 October. These measurements were the first stellar occultation of Mars in the EUV wavelengths (90-110 nm). Due to the higher sensitivity of the EMUS instrument, the occultation measurements were able to probe the atmosphere with an altitude sampling of 2 km or lower. The occultation measurements by SPICAM/MEx and IUVS/MAVEN were limited to 160 km due to wavelengths limited to a longward of 110 nm. However, the use of EUV wavelengths in the EMUS stellar occultation provided atmospheric probing up to 190 km thus enabling neutral density retrieval up to the exobase region of Mars. The CO2 densities are retrieved from 90-185 km and the temperature profiles were retrieved using the constraint of hydrostatic equilibrium to the CO2 densities. We shall discuss results from the EMUS occultation campaign specifically the observed variability in the CO2 density and temperature during the occultation campaign.

COVID-19 is arguably the biggest health crisis the world has faced in the 21st century. Therefore, two of the polyherbal formulations, Infuza and Kulzam were assessed for the prevention of COVID-19 infection as a repurposed medication. Four hundred seven high-risk subjects were recruited in the present open-label randomized controlled clinical trial for eligibility. After assessment for eligibility, remaining 251 subjects were randomized to the test and control groups. Further, 52 high-risk subjects in Infuza, 51 in Kulzam, 51 in InfuzaKulzam and 53 in control group completed the 14 days of intervention/assessment. The phenotyping of lymphocytes at baseline (0 day) and after 14 days of treatment was carried out by flow cytometry assays. A total of 15.09% high-risk subjects in control group turned positive as compared to only 7.69% in Infuza, 3.92% in Kulzam and 1.96% in InfuzaKulzam groups. The rate of conversion to COVID-19 infection in InfuzaKulzam group was minimal and statistically significant as compared to control group (p0.017). No significant changes in phenotype of lymphocytes (T, B, NK cells), absolute lymphocyte count and cytokine levels were found in study groups. However, there was a decreasing trend of hs-CRP level in high-risk subjects after intervention of polyherbal formulations for 14 days. The combination of Infuza and Kulzam may synergistically prevent COVID-19 infection in high-risk subjects of COVID-19.

Introduction: Type of materials used in fabrication of denture base has an effect on dimension during denture base material processing and other factors related to clinical use. The study aims were to assess the efficiency of complete dentures made using bps, lecutonite & acrylic materials. Material and Methods: Ninety patients were selected to construct complete dentures with bps, lecutonite & acrylic materials denture base materials. They were randomly divided into three groups: group 1, patients with bps; group 2, patients with heat curing acrylic resin fabricated by injection moulding technique and conventional methods; and group 3, patients with lecutonite. The dimensional changes were assessed using digital caliper. Results: After the twelfth month, injection moulding acrylic resin had significantly the highest dimensional change followed by the lecutonite. There were no significant differences in the dimensions between the three types of denture base materials at normal mouth temperature, while, after hot tea drinking at 45∘C, the dimensional change was significantly the highest in cobalt chrome metallic denture base group. Conclusion: BPS denture base has stable dimension compared to denture bases fabricated of lecutonite, acrylic resin but it was more affected by altered mouth temperature.

Acromioclavicular joint tuberculosis is an extremely rare presentation with only 16 cases reported so far and has a relatively high propensity to be misdiagnosed. India being a tuberculosis endemic region accounts for almost 27% of cases worldwide (global index of 2018 was 10 million). With a higher index of suspicion an earlier diagnosis can be made. We report two patients of AC joint tuberculosis, treated with multidrug chemotherapy resulting in a good functional outcome.

The Imaging UltraViolet Spectrograph (IUVS) (McClintock et al., 2015) onboard the MAVEN (Mars Atmosphere and Volatile EvolutioN) spacecraft performs limb observations of the Mars atmosphere in the dayside. Spectra have been acquired in the ultraviolet domain, between and 110 and 340 nm, since September 2014. Additionally, the UVIS (UV and Visible Spectrometer) channel of the NOMAD (Nadir and Occultation for MArs Discovery) spectrometer (Patel et al., 2017; Vandaele et al., 2018) onboard the ExoMars Trace Gas Orbiter has performed the same type of observations both in the middle ultraviolet and the visible domains (200 – 650 nm), since April 2019. It is the first instrument that allows studying UV and visible emissions simultaneously that can, thus, be directly compared. The visible emissions of the oxygen green line (557.7 nm, Gérard et al., 2020) and the oxygen red line doublet (630.0-636.4 nm, Gérard et al., 2021) have already been investigated by Soret et al. (2022), using the NOMAD/UVIS data. The variation of their peak brightness and altitudes have been studied over seasons and compared to photochemical model simulations. In this work, we present the ultraviolet dayglow counterpart of the visible dayglow and compare the results of both the NOMAD/UVIS and MAVEN/IUVS instruments. The [OI] 297.2 nm emission that, like the oxygen green line, originates from the O(1S) state is analyzed. The [OI] 297.2 nm has already been extensively studied with the IUVS instrument (Gkouvelis et al., 2018) but it is the first time that both the 297.2 and 557.7 nm can be observed simultaneously, with NOMAD/UVIS. The correlation of those emissions is shown and the ratio I(557.7 nm)/I(297.2 nm) is established with NOMAD/UVIS concurrent measurements. The CO2+ UVD and CO Cameron bands, that have been studied with the MAVEN/IUVS instrument are also presented and compared to UVIS observations. Finally, the CO2+ Fox-Duffendack-Barker (FDB) system, that has not been observed on Mars since Mariner, is also investigated. We present averaged limb profiles of all these ultraviolet emissions, their seasonal variations and ratios of their brightness. References: Gérard, J. C. et al. (2020), Detection of green line emission in the dayside atmosphere of Mars from NOMAD-TGO observations. Nature Astronomy, 4(11), 1049-1052 Gérard, J. C. et al. (2021), First observation of the oxygen 630 nm emission in the Martian dayglow. Geophysical Research Letters, 48(8), e2020GL092334, https://doi.org/10.1029/2020GL092334 Gkouvelis, L., et al. (2018), The O(1S) 297.2-nm dayglow emission: a tracer of CO2 density variations in the Martian lower thermosphere. Journal of Geophysical Research: Planets, 123(12), 3119-3132 McClintock, W. E. et al. (2015), The Imaging Ultraviolet Spectrograph (IUVS) for the MAVEN mission. Space Science Reviews, 195(1–4), 75–124. https://doi.org/10.1007/s11214-014-0098-7 Patel, M. R. et al. (2017), NOMAD spectrometer on the ExoMars trace gas orbiter mission: part 2—design, manufacturing, and testing of the ultraviolet and visible channel. Applied optics, 56(10), 2771-2782. https://doi.org/10.1364/AO.56.002771 Soret, L. et al. (2022), The Mars oxygen visible dayglow: a Martian year of NOMAD/UVIS observations, Journal of Geophysical Research Vandaele, A. C. et al. (2018), NOMAD, an integrated suite of spectrometers for the ExoMars Trace Gas Mission: Technical description, science objectives, and expected performance. Space Science Reviews, 214(5). https://doi.org/10.1007/s11214-018-0517-2

The spin-forbidden CO a 3Π→ X 1Σ Cameron bands (190-270 nm) are the dominant feature of the middle ultraviolet spectrum of the Martian dayglow and aurora. Since their discovery in the Mars dayglow during the Mariner era (Barth, 1969), a number of studies based on observations with the SPICAM instrument on board the Mars Express (Leblanc et al., 2006; Cox et al., 2010; González‐Galindo et al., 2018) and IUVS/MAVEN (Jain et al., 2015) have revealed their altitude distribution and seasonal changes (Gérard et al., 2019). The Cameron bands are also an important marker of the distribution of auroral events on the nightside aurora, together with the CO2+ ultraviolet doublet at 288-289 nm (Gérard et al., 2015; Schneider et al., 2015). One of the important processes producing the metastable a 3Π upper state of the transition is dissociative excitation of CO2 by impact of photoelectrons or auroral electrons: e (E> 11.5 eV) + CO2 à CO (a 3Π) + O + e The excitation process includes cascades from higher lying states, which makes ab initio calculations quite complex. Until recently, models for the production of the Cameron bands used the energy dependence of the cross section initially published by Ajello (1971) 50 years ago. It was later normalized by Avakyan et al. (1999) to the value of Erdman and Zipf (1983) at 80 eV. The absolute value of the cross section was later scaled by different factors to account for revisions of the radiative lifetime of the a3Π state and match the observations. Recently, a new set of measurements in a large laboratory facility attenuating the wall effects has led to a revision of both the shape and the peak value of this cross section (Lee et al., 2021a). In this presentation, we assess the consequences of this revision on the production of the Cameron bands in the Martian airglow and aurora. In particular, we discuss the importance of the contribution of the excitation of CO by electron impact e (E> 6 eV) + CO → CO(a 3Π) + e, also recently re-examined by Lee et al. (2021b). We discuss the relative importance of the two processes and its dependence on the CO mixing ratio in the Mars thermosphere. We also examine how these new values may affect the anomalies in the Cameron/CO2+ UV doublet intensity ratio observed with IUVS in the discrete aurora (Soret et al., 2021). References Ajello, J. M. (1971). The Journal of Chemical Physics, 55(7), 3169-3177. Avakyan, S. V. et al. (1999). CRC Press. Barth, C. A. et al. (1969). Science, 165(3897), 1004-1005. Cox, C. et al. (2010). Journal of Geophysical Research: Planets, 115(E4). Erdman, P. W., & Zipf, E. C. (1983). Planetary and Space Science, 31(3), 317-321. Gérard, J. C. et al. (2019). Journal of Geophysical Research: Space Physics, 124(7), 5816-5827. González‐Galindo, F. et al. (2018). Journal of Geophysical Research: Planets, 123(7), 1934-1952. Jain, S. K. et al. (2015). Geophysical Research Letters, 42(21), 9023-9030. Leblanc, F. et al. (2006). Journal of Geophysical Research: Planets, 111(E9). Lee, R., et al. (2021a). Mars and Venus dayglow studies based upon laboratory aeronomy from electron Impact of CO2 for analysis of UV Observations by MAVEN, EMM, MEx, and VEx. AGU Fall meeting 2021, New Orleans. Lee, R. A. et al. (2021b). Journal of Geophysical Research: Planets, 126(1), e2020JE006602. Schneider, N. M. et al. (2015). Discovery of diffuse aurora on Mars. Science, 350(6261), aad0313. Soret, L. et al. (2021). Journal of Geophysical Research: Space Physics, 126(10), e2021JA029495.

Since the discovery of atmospheric Mg+ at Mars in 2015 by the Mars Atmosphere and Volatile Evolution (MAVEN) mission, there have been almost continuous observations of this meteoric ion layer in a variety of seasons, local times, and latitudes. Here we present the most comprehensive set of observations of the persistent metal ion layer at Mars, constructing the first grand composite maps of a metallic ion species. These maps demonstrate that Mg+ appears in almost all conditions when illuminated, with peak values varying between 100 and 500 cm-3, dependent on season and local time. There exists significant latitudinal variation within a given season, indicating that Mg+ is not simply an inert tracer, but instead may be influenced by the meteoric input distribution and/or atmospheric dynamics and chemistry. Geographic maps of latitude and longitude indicate that Mg+ may be influenced by atmospheric tides, and there is no apparent correlation with remnant crustal magnetic fields. This work also presents counter-intuitive results, such as a reduction of Mg+ ions in the northern hemisphere during Northern Winter in an apparent correlation with dust aerosols.

Here we report on synoptic (or “disk”) observations of Martian discrete aurora in the extreme and far ultraviolet (

Water is lost from the Mars upper atmosphere to space as hydrogen and oxygen, both of which can be observed in scattered ultraviolet sunlight at 102.6 nm. We present Emirates Mars Mission Emirates Mars Ultraviolet Spectrometer (EMM/EMUS) insertion orbit observations of this airglow, resolving the independent altitude contributions of H and O for the first time. We present the first airglow modeling of the complete H and O 102.6 nm system and the first 3D azimuthally symmetric modeling of the O emission, retrieving temperatures and densities typical of northern spring. Our model reproduces the emission well above 200 km, but does not incorporate partial frequency redistribution needed to reproduce the observed O brightness at lower altitudes and on the disk. These results support future EMM/EMUS science orbit retrievals of H loss and the use of 102.6 nm observations to constrain planetary atmospheres across the solar system. UAE government; EMM/MBRSC; NASA through the MAVEN mission; KU-CU-LASP Space Sci. [8474000332] Published version Funding for development of the EMM mission was provided by the UAE government, and to co-authors outside of the UAE by MBRSC. Funding for the development of the radiative transfer model was provided by EMM/MBRSC and by NASA through the MAVEN mission. SR and KC are supported by the grant 8474000332-KU-CU-LASP Space Sci.