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The Aditya-L1 mission of ISRO
The Aditya-L1 is the first space-based solar observatory of the Indian Space Research Organization (ISRO). The spacecraft will carry seven payloads providing uninterrupted observations of the Sun from the first Lagrangian point. Aditya-L1 comprises four remote sensing instruments, viz. a coronagraph observing in visible and infrared, a full disk imager in Near Ultra-Violet (NUV), and two full-sun integrated spectrometers in soft X-ray and hard X-ray. In addition, there are three instruments for in-situ measurements, including a magnetometer, to study the magnetic field variations during energetic events. Aditya-L1 is truly a mission for multi-messenger solar astronomy from space that will provide comprehensive observations of the Sun across the electromagnetic spectrum and in-situ measurements in a broad range of energy, including magnetic field measurements at L1.
Journal Article
The sun
\"Simple text and full-color photographs describe the Sun\"-- Provided by the publisher.
Book
Sun protection behavior beliefs among adults living in rural United States: A qualitative study in Minnesota
Although skin cancers are considered mostly preventable, more people in the US are diagnosed with skin cancer than all other cancers combined. Sun safety recommendations include wearing sun-protective clothing, a wide-brimmed hat, seeking shade, and using sunscreen. Some evidence exists that sun risk behaviors and skin cancer rates are more frequent among rural than urban US populations, raising questions about underlying factors. We conducted a belief elicitation survey on these four sun protection behaviors among 278 adults (aged 18–60 years) living in rural Minnesota, a state with high sunburn rates and UV-attributable melanoma cases. These qualitative data were analyzed using content analysis, and the identified codes ranked by frequency. Almost all participants emphasized that spending time outside was important to them. The most frequently reported sun protection behaviors were wearing sunscreen and protective clothing. The primary outcomes were obtained from open-ended questions on outcome, normative, and control beliefs associated with each sun protection behavior. While many different beliefs were mentioned, reducing sunburn and skin cancer risk were commonly reported across all behaviors. Beliefs about negative aspects of each behavior (e.g., interference with being physically active or doing work outside, greasy/sticky sunscreen, not getting a suntan, overheating in long clothes or when wearing hats, hats that blow off easily) typically outnumbered positive aspects (e.g., protective behaviors enabling being outside, staying cool in shade, reduced skin aging). The majority of participants believed that most people would approve of all protection behaviors, but many thought that age was a factor for behavior adoption, with young people typically thought to engage less in protective behaviors. Some commonly reported negative aspects of sun protective behaviors were related to activities more common in rural populations, such as working outside. This suggests that rural sun protection promotion may include structural interventions to make sun protection easy, convenient, and accessible without impeding rural lifestyles.
Journal Article
Decoding the Pre-Eruptive Magnetic Field Configurations of Coronal Mass Ejections
A clear understanding of the nature of the pre-eruptive magnetic field configurations of Coronal Mass Ejections (CMEs) is required for understanding and eventually predicting solar eruptions. Only two, but seemingly disparate, magnetic configurations are considered viable; namely, sheared magnetic arcades (SMA) and magnetic flux ropes (MFR). They can form via three physical mechanisms (flux emergence, flux cancellation, helicity condensation). Whether the CME culprit is an SMA or an MFR, however, has been strongly debated for thirty years. We formed an International Space Science Institute (ISSI) team to address and resolve this issue and report the outcome here. We review the status of the field across modeling and observations, identify the open and closed issues, compile lists of SMA and MFR observables to be tested against observations and outline research activities to close the gaps in our current understanding. We propose that the combination of multi-viewpoint multi-thermal coronal observations and multi-height vector magnetic field measurements is the optimal approach for resolving the issue conclusively. We demonstrate the approach using MHD simulations and synthetic coronal images.
Our key conclusion is that the differentiation of pre-eruptive configurations in terms of SMAs and MFRs seems artificial. Both observations and modeling can be made consistent if the pre-eruptive configuration exists in a hybrid state that is continuously evolving from an SMA to an MFR. Thus, the ‘dominant’ nature of a given configuration will largely depend on its evolutionary stage (SMA-like early-on, MFR-like near the eruption).
Journal Article
Let's explore the sun
\"Did you know that the sun is actually a star? As the closest star to Earth, the sun provides light and warmth to our planet every day! Learn more about what makes this star special, through vibrant photos and carefully leveled text.\"--Amazon.com.
Book
Solar Ultraviolet Bursts
The term “ultraviolet (UV) burst” is introduced to describe small, intense, transient brightenings in ultraviolet images of solar active regions. We inventorize their properties and provide a definition based on image sequences in transition-region lines. Coronal signatures are rare, and most bursts are associated with small-scale, canceling opposite-polarity fields in the photosphere that occur in emerging flux regions, moving magnetic features in sunspot moats, and sunspot light bridges. We also compare UV bursts with similar transition-region phenomena found previously in solar ultraviolet spectrometry and with similar phenomena at optical wavelengths, in particular Ellerman bombs. Akin to the latter, UV bursts are probably small-scale magnetic reconnection events occurring in the low atmosphere, at photospheric and/or chromospheric heights. Their intense emission in lines with optically thin formation gives unique diagnostic opportunities for studying the physics of magnetic reconnection in the low solar atmosphere. This paper is a review report from an International Space Science Institute team that met in 2016–2017.
Journal Article
Multiwavelength Studies of MHD Waves in the Solar Chromosphere
The chromosphere is a thin layer of the solar atmosphere that bridges the relatively cool photosphere and the intensely heated transition region and corona. Compressible and incompressible waves propagating through the chromosphere can supply significant amounts of energy to the interface region and corona. In recent years an abundance of high-resolution observations from state-of-the-art facilities have provided new and exciting ways of disentangling the characteristics of oscillatory phenomena propagating through the dynamic chromosphere. Coupled with rapid advancements in magnetohydrodynamic wave theory, we are now in an ideal position to thoroughly investigate the role waves play in supplying energy to sustain chromospheric and coronal heating. Here, we review the recent progress made in characterising, categorising and interpreting oscillations manifesting in the solar chromosphere, with an impetus placed on their intrinsic energetics.
Journal Article