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Biospherian handshake: Mark Nelson with John Allen (left), inventor and Ex- ecutive Chairman of the Biosphere 2 project and Academician Oleg Gazenko, Director, Institute of Biomedical Problems, Moscow (photo by Abigail Alling, Biosphere 2, 1991–1993).
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Successfully managing group dynamics of small, physically isolated groups is vital for long duration space exploration/habitation and for terrestrial CELSS (Controlled Environmental Life Support System) facilities with human participants. Biosphere 2 had important differences and shares some key commonalities with both Antarctic and space environme...
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... the glass. Efforts to ensure privacy when needed included private crew bedrooms (which other crew needed permission to enter). The entire habitat area occupied the second floor out of view of visitors, private phone lines, computers for sending/receiv- ing email. Interior space and dense growth in biomes also provided privacy in secluded locations. 9. Social valency, personality conflicts and cabin fever . Scientists have observed that larger crew sizes enhance social diversity but increase the danger of schisms and subgroup factions (ISU, 2009). The Biosphere 2 crew worked together extensively during training and came in as friends, in some cases long-term friends, but tensions inside split the group. Nevertheless, they had to work together on many tasks, share some 2200 meals together, and in- teract daily with the same group of seven others. The two groups which cohered better socially took opposite sides of the management conflict. Cabin fever refers to annoyances that can build up when there is no escape. Admiral Byrd noted: “I knew of one who could not eat unless he could find a place in the mess hall out of view of a [person] who solemnly chewed twenty-eight times before swallowing. In a polar camp, little things like that have the power to drive even disciplined men to the brink of insani- ty” (Byrd, 1938). 10. Oxygen decline, elevated carbon dioxide . Amongst the most unexpected and interesting occurrences of the first two years was a gradual decline in oxygen, falling from 20.9% to around 14% over the first sixteen months (Severinghaus et al., 1994; Nelson and Dempster, 1996). Probably because atmospheric pressure did not change, there could not be the same adaptation as in mountain- climbers. Several crew developed sleep apnea (though supple- mented by oxygen lines run to their bedrooms at night from the analytic laboratory) and, coupled with the caloric restricted diet, this diminished energy and possibly cognitive abilities (Walford and Spindler, 1997; Walford et al., 1996) until oxygen was replen- ished 16 months into the closure. Carbon dioxide levels were much higher than ambient, reaching highs of over 4000 ppm during win- ter months (Nelson and Dempster, 1996). These levels are compa- rable to Space Shuttle at 5000–10,000 ppm and International Space Station levels at under 2000 to 9000 ppm (James et al., 2011). 11. Sex/gender . There were four women and four men in the crew. There were two couples who bonded before entry (and remain together twenty years after the closure experiment). Two individuals were in no sexual relationship, and two left partners outside. The tensions underlying actual and fantasized sexual li- aisons or attractions – jealousy, intrigue – always powerful in human groupings, perhaps grow more so in isolated, confined groups. Psychological studies on male Antarctic and submarine crews were one of the vectors that led to a decision for an equal gender mix in Biosphere 2. Including women has been found to relieve pressure and help normalize the culture of isolated groups. Women perform as well or better than men in these circumstances (Connors et al., 1985). 1. Perceived historic importance of undertaking . Studies of submarine crew demonstrate that people selected for challenging environments are highly motivated to perform in very difficult circumstances (Helmreich, 1974). The biospherians had volunteered and competed with a larger group of candidates for the privi- lege of carrying out the unprecedented closure experiments. They had extensive training and were key participants in the construction, botanical/animal collections and preparations for the experiment. As has been noted of astronauts and other expeditionary crew, belief that what one is doing is of historic importance of- ten influences the willingness to deal with hardship and stress (Suedfeld, 1991). The “heroic mode” can also lead to people push- ing themselves past their maximum (Allen, 2002). 2. Diversity of shared and private spaces within Biosphere 2 . For a confined environment, the facility offered relatively spacious and attractive locations for both shared and private functions (these are detailed in Alling et al., 2002). Bechtel et al. (1997) identified some 50 behavior settings and found that each biospherian had 3.5 behavior settings, more than three times that available to the population of a small town. Each had a personal apartment with upstairs sleeping loft and downstairs living room. 3. Communications with the outside . The closure experiments (1991–1994) coincided with early years of the Internet, and email and video linkups with Mission Control and consulting scientists and engineers were available. Telephones were installed at a place where crew could speak with friends/family. Evolution of communications change the nature of isolation and confinement. So while only eight people lived inside Biosphere 2, biospherians main- tained a complex social life through meetings at the glass (Fig. 4) and digital communications. 4. Creative expressions through the arts . The biospherians painted, wrote poetry, performed music and pursued photogra- phy/video. One crew member did an electronic link with a performance artist traveling around the world during the two year closure. There were occasions when the biospherians held “inter- biospheric arts festivals” presenting their work and listening, see- ing the work of outside artists (Fig. 5). Many kept journals, wrote scientific and popular papers and books including a cook book of the best recipes (Silverstone, 1993). 5. Public and school support . Biospherians got morale boosts interacting with enthusiastic and supportive visitors. They did linkups with school groups – from K-12 to university groups – either with those directly outside the facility (linked by 2-way radios) or via phone. 6. Nature and beauty . Biosphere 2 was designed to be beautiful and awe-inspiring. Minimizing or eliminating off-gassing of materials was a design priority. The interiors utilized natural fibers and wood wherever possible, and the healing effect of being sur- rounded by luxuriant vegetation helped mitigate the feeling that the crew was deprived and isolated. A growing body of evidence supports the health and psychological benefits of an environment with green plants (Clay, 2001). The environment was pollution- free compared to urban settings. There was more natural diversity encountered inside Biosphere 2 than is available to most people (Fig. 6). 7. Feeling yourself a vital part of a larger whole . As space crews also reported, the biospherians felt like they could respond to whatever their world needed – changing irrigation times, maintaining and repairing equipment, preventing invasive species from over-running areas of the biomes, working to maximize use of “sunfall” with additional plantings to counteract CO 2 rise and increase food supply. Connectedness of all vectors was an important factor in why Biosphere 2 could operate – and the feeling of being able to respond empowers. Each biospherian reported a deep sense of being part of a living system. The crew were caretakers, keeping machinery going to ensure water availability, temperature control, etc. They also realized that without their ecosystem, they would not survive. Understanding that Biosphere 2 was the crew’s “life boat” (life support system) may have helped the success of the mission. The crew understood that “the health of the biosphere is synonymous with our health” (Alling and Nelson, 1993). The Biosphere 2 crew, for the first closure experiment, ranged in age from 29 to 67, from different socio-economic backgrounds, from technically skilled high school graduates to graduate level professionals and medical doctor. Five were from the US, two from the UK and one from Belgium. All candidates received extensive and intensive training prior to the closure. They had all worked in small group settings at various remote settings such as Institute of Ecotechnics-consulted projects in West Australia and aboard an ocean-going ship learning mar- itime skills, and creating and performing theatrical pieces. They had also worked at the Biosphere 2 facility during construction, operating the onsite prototype farm and other systems developed for the facility. They started with others in a larger group of biospherian candidates, and finally trained as a team preparing for the closure experiment. An important tool for dealing with group dynamics in Biosphere 2 was familiarity with the work of W.R. Bion who studied small group behavior (Allen, 2002). Working at the Tavistock Clinic in the UK in the 1940s, he worked with “shell-shocked” (the then current term for post traumatic stress disorder) pilots relieved of duty during World War 2. The objective was to see if they could return to health and rejoin their combat unit. Bion demonstrated that a small group operates under specific patterns of behavior differing from individuals or large groups. This unconsciously generated behavior, unless brought to light, defeat a task group’s commitment to achieve their purpose. Specifically he discovered three sets of unconscious behavior in small groups (Bion, 1961). These operate during “group animal” mode, as op- posed to the “task group” mode, which carries out their accepted task, and can be short-lived or can operate for extended periods of time when the group has lapsed off-task. All three of these behavior patterns sabotage the task. One dysfunctional characteristic is an unrealistic treatment of resources and the time needed for completion of tasks. (1) Fight/Flight, in which the group alternates between fighting, and fleeing from the task. This manifests in a myriad of ways such as not showing up at meetings or constant arguing about strategy and purpose. (2) Pairing, in which the group abdicates leadership and think- ing to a twosome, then passively waits for that pair to decide what the group should do. (3) ...
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... and consulting scientists and engineers were available. Telephones were installed at a place where crew could speak with friends/family. Evolution of commu- nications change the nature of isolation and confinement. So while only eight people lived inside Biosphere 2, biospherians main- tained a complex social life through meetings at the glass (Fig. 4) and digital communications. . Creative expressions through the arts. The biospherians painted, wrote poetry, performed music and pursued photogra- phy/video. One crew member did an electronic link with a per- formance artist traveling around the world during the two year closure. There were occasions when the biospherians held "inter- ...
Citations
... Realizing that it was our life boat led to a high degree of mindfulness about any action we considered undertaking. The beauty of the world we were living in and our physical, emotional bonding with it were sources of great satisfaction and helped hold the crew together despite an outside power struggle and internal frictions (Nelson, 2018;Nelson et al., 2015) (Figure 4). ...
The Biosphere 2 project, a 1.2 hectare materially-closed mini-biosphere which supported teams of biospherian crews from 1991-1994 provides a host of ecological and human-biosphere lessons relevant to our global biospheric challenges. Because of its high visibility through worldwide media coverage, the project advanced public understanding of what a biosphere is and the roles that humans can constructively play in keeping ecosystems and atmosphere healthy. The present paper touches on the fairly recent scientific understanding of our global biosphere and some of the intriguing results from Biosphere 2. It also examines some of the reasons that Biosphere 2 aroused controversy because of narrow definitions and expectations of how science is to be conducted. The cooperation between engineers and ecologists and the requirement to design a technosphere for Biosphere 2 that supported the life inside without harming it has enormous relevance to what is required in our global home. There was an unexpected and profound connection that the “biospherian” crew inside Biosphere 2 felt to their living biosphere. Biosphere 2 also demonstrated new kinds of roles that can be played by people aware of a biosphere as their life support system.
... We have a limited view on how the UV sky looks because of the lack of current UV missions. This spectral region has a special significance in astronomy as it contains a wealth of information on the physical properties of gas, stars and galaxies (Côté, 2014). Indeed, this region is critically important for characterizing the emission from young and/or hot stars, as well as from hard non-thermal sources. ...
Though the ultraviolet (UV) domain plays a vital role in the studies of astronomical transient events, the UV time-domain sky remains largely unexplored. We have designed a wide-field UV imager that can be flown on a range of available platforms, such as high-altitude balloons, CubeSats, and larger space missions. The major scientific goals are the variability of astronomical sources, detection of transients such as supernovae, novae, tidal disruption events, and characterizing AGN variability. The instrument has an 80 mm aperture with a circular field of view of 10.8 degrees, an angular resolution of around 22 arcsec, and a 240-390 nm spectral observation window. The detector for the instrument is a Microchannel Plate (MCP)-based image intensifier with both photon counting and integration capabilities. An FPGA-based detector readout mechanism and real-time data processing have been implemented. The imager is designed in such a way that its lightweight and compact nature are well fitted for the CubeSat dimensions. Here we present various design and developmental aspects of this UV wide-field transient explorer.
... A crude estimate of the possible radio flux density of an exoplanet can be made by simply scaling the known values of Jupiter to nearby stellar distances. Jupiter is the strongest radio emitter of the solar system planets and at 15 MHz has a peak flux density of S ν ∼ 10 10 mJy ( Zarka 1992). If Jupiter were at the distance of a relatively nearby star at 10 pc, it would have a peak flux density of only S ν ∼ 0.07 mJy at 15 MHz, which is too faint to be detectable with existing radio observatories. ...
The majority of searches for radio emission from exoplanets have to date focused on short period planets, i.e., the so-called hot Jupiter type planets. However, these planets are likely to be tidally locked to their host stars and may not generate sufficiently strong magnetic fields to emit electron cyclotron maser emission at the low frequencies used in observations (typically >150 MHz). In comparison, the large mass-loss rates of evolved stars could enable exoplanets at larger orbital distances to emit detectable radio emission. Here, we first show that the large ionized mass-loss rates of certain evolved stars relative to the solar value could make them detectable with the Low Frequency Array (LOFAR) at 150 MHz ($\lambda$ = 2 m), provided they have surface magnetic field strengths >50 G. We then report radio observations of three long period (>1 au) planets that orbit the evolved stars $\beta$ Gem, $\iota$ Dra, and $\beta$ UMi using LOFAR at 150 MHz. We do not detect radio emission from any system but place tight 3$\sigma$ upper limits of 0.98, 0.87, and 0.57 mJy on the flux density at 150 MHz for $\beta$ Gem, $\iota$ Dra, and $\beta$ UMi, respectively. Despite our non-detections these stringent upper limits highlight the potential of LOFAR as a tool to search for exoplanetary radio emission at meter wavelengths.
... Cohen et al. 2015;Garraffo et al. 2017;Wheatley et al. 2017). Coherent, nonthermal radio emission attributed the electron-cyclotron maser instability (ECMI) is observed at magnetised planets in the solar system and is associated with auroral activity ( Wu & Lee 1979;Zarka 1992;Ergun et al. 2000;Treumann 2006;Imai et al. 2008). Although auroral emission from exoplanets has yet to be detected (e.g. ...
... The 'Radiometric Bode's Law' (RBL) is an empirical scaling relation based on observations of radio emission from magnetised Solar System planets that is often extrapolated to estimate the radio power expected from exoplanets (e.g. Lazio et al. 2004;Zarka 2007). The RBL relates the output radio power from a planetary body to the Poynting or kinetic energy flux convected onto the obstacle, and has been used to demonstrate that hot Jupiters may be detectable with the next generation of radio telescopes ( Farrell et al. 2004;Lazio et al. 2004;Grießmeier et al. 2007;Zarka 2007). ...
... Lazio et al. 2004;Zarka 2007). The RBL relates the output radio power from a planetary body to the Poynting or kinetic energy flux convected onto the obstacle, and has been used to demonstrate that hot Jupiters may be detectable with the next generation of radio telescopes ( Farrell et al. 2004;Lazio et al. 2004;Grießmeier et al. 2007;Zarka 2007). However, the RBL is empirical in nature and emission driven by ionospheric flow resulting from the reconnection of interplanetary and exoplanetary magnetic fields, analogous to the process generating Earth's auroral radio emission, has also been studied ( Nichols & Milan 2016), and is predicted to be detectable with the next generation of radio telescopes. ...
We consider the magnetic interaction of exoplanets orbiting M-dwarfs, calculating the expected Poynting flux carried upstream along Alfv\'{e}n wings to the central star. A region of emission analogous to the Io footprint observed in Jupiter's aurora is produced, and we calculate the radio flux density generated near the surface of the star via the electron-cyclotron maser instability. We apply the model to produce individual case studies for the TRAPPIST-1, Proxima Centauri, and the dwarf NGTS-1 systems. We predict steady-state flux densities of up to ~ 10 $\mu$Jy and sporadic bursts of emission of up to ~ 1 mJy from each case study, suggesting these systems may be detectable with the Very Large Array (VLA) and the Giant Metrewave Radio Telescope (GMRT), and in future with the Square Kilometre Array (SKA). Finally, we present a survey of 85 exoplanets orbiting M-dwarfs, identifying 11 such objects capable of generating radio emission above 10 $\mu$Jy.
... The temperature rise above the photosphere is accompanied by an increase in the nonthermal (turbulence) velocity. Profiles of the chromospheric and TR lines have been analyzed to measure the temperature and nonthermal velocities as well as the electron density (Tandberg-Hanssen 1960;Kjeldseth Moe & Nicolas 1977;Lemaire 2007). The TR lines usually show some degree of asymmetry as well as a large line width far in excess of their thermal broadening. ...
Context. Light bridges (LBs) are elongated structures with enhanced intensity embedded in sunspot umbra and pores.
Aims. We studied the properties of a sample of 60 LBs observed with the Interface Region Imaging Spectrograph (IRIS).
Methods. Using IRIS near- and far-ultraviolet spectra, we measured the line intensity, width, and Doppler shift; followed traces of LBs in the chromosphere and transition region (TR); and compared LB parameters with umbra and quiet Sun.
Results. There is a systematic emission enhancement in LBs compared to nearby umbra from the photosphere up to the TR. Light bridges are systematically displaced toward the solar limb at higher layers: the amount of the displacement at one solar radius compares well with the typical height of the chromosphere and TR. The intensity of the LB sample compared to the umbra sample peaks at the middle/upper chromosphere where they are almost permanently bright. Spectral lines emerging from the LBs are broader than the nearby umbra. The systematic redshift of the Si iv line in the LB sample is reduced compared to the quiet Sun sample. We found a significant correlation between the line width of ions arising at temperatures from 3 × 10 ⁴ to 1.5 × 10 ⁵ K as there is also a strong spatial correlation among the line and continuum intensities. In addition, the intensity−line width relation holds for all spectral lines in this study. The correlations indicate that the cool and hot plasma in LBs are coupled.
Conclusions. Light bridges comprise multi-temperature and multi-disciplinary structures extending up to the TR. Diverse heating sources supply the energy and momentum to different layers, resulting in distinct dynamics in the photosphere, chromosphere, and TR.
... We then calculated the squashing factor Q in the box volume of the potential field with the code introduced by Liu et al. (2016b). The reason to use a potential field model instead of an NLFFF is that structural skeletons of magnetic field are very robust as demonstrated by many earlier studies (e.g., Démoulin 2006Démoulin , 2007Liu et al. 2014). ...
We report the intriguing large-scale dynamic phenomena associated with the M6.5 flare~(SOL2015-06-22T18:23) in NOAA active region 12371, observed by RHESSI, Fermi, and the Atmospheric Image Assembly (AIA) and Magnetic Imager (HMI) on the Solar Dynamic Observatory (SDO). The most interesting feature of this event is a third ribbon (R3) arising in the decay phase, propagating along a dimming channel (seen in EUV passbands) towards a neighboring sunspot. The propagation of R3 occurs in the presence of hard X-ray footpoint emission, and is broadly visible at temperatures from 0.6~MK to over 10~MK through the Differential Emission Measure (DEM) analysis. The coronal loops then undergo an apparent slipping motion following the same path of R3, after a $\sim$ 80~min delay. To understand the underlying physics, we investigate the magnetic configuration and the thermal structure of the flaring region. Our results are in favor of a slipping-type reconnection followed by the thermodynamic evolution of coronal loops. In comparison with those previously reported slipping reconnection events, this one proceeds across a particularly long distance ($\sim$60 Mm) over a long period of time ($\sim$50 min), and shows two clearly distinguished phases: the propagation of the footpoint brightening driven by nonthermal particle injection and the apparent slippage of loops governed by plasma heating and subsequent cooling.
... In the 3D framework, magnetic reconnection takes place preferentially at a separator (intersection of two separatrices; Baum & Bratenahl 1980;Lau & Finn 1990;Longcope & Cowley 1996;Longcope 2005) or at its generalization, a hyperbolic flux tube (HFT; intersection of two quasi-separatrix layers, or QSLs; Démoulin et al. 1996Démoulin et al. , 1997Titov et al. 2002). The 3D magnetic reconnection is manifest in many two-ribbon flare observations (Gorbachev & Somov 1988;Mandrini et al. 1991;Démoulin et al. 1993;Démoulin 2007), such as bi-directional spread of post-flare arcade (Aulanier et al. 2007), anti-parallel motions of hard X-ray sources (Aulanier et al. 2006;Démoulin 2007), elongation motion of flare ribbons (Qiu et al. 2002(Qiu et al. , 2010Qiu 2009;Fletcher et al. 2004), and J-shaped flare ribbons (Aulanier et al. 2012). Besides two-ribbon flares, circular-ribbon flares also exhibit a special configuration of 3D magnetic reconnection with a null point and a fan-spine structure (Masson et al. 2009;Sun et al. 2013;Yang et al. 2015). ...
... In the 3D framework, magnetic reconnection takes place preferentially at a separator (intersection of two separatrices; Baum & Bratenahl 1980;Lau & Finn 1990;Longcope & Cowley 1996;Longcope 2005) or at its generalization, a hyperbolic flux tube (HFT; intersection of two quasi-separatrix layers, or QSLs; Démoulin et al. 1996Démoulin et al. , 1997Titov et al. 2002). The 3D magnetic reconnection is manifest in many two-ribbon flare observations (Gorbachev & Somov 1988;Mandrini et al. 1991;Démoulin et al. 1993;Démoulin 2007), such as bi-directional spread of post-flare arcade (Aulanier et al. 2007), anti-parallel motions of hard X-ray sources (Aulanier et al. 2006;Démoulin 2007), elongation motion of flare ribbons (Qiu et al. 2002(Qiu et al. , 2010Qiu 2009;Fletcher et al. 2004), and J-shaped flare ribbons (Aulanier et al. 2012). Besides two-ribbon flares, circular-ribbon flares also exhibit a special configuration of 3D magnetic reconnection with a null point and a fan-spine structure (Masson et al. 2009;Sun et al. 2013;Yang et al. 2015). ...
We report evolution of an atypical X-shaped flare ribbon which provides novel observational evidence of three-dimensional (3D) magnetic reconnection at a separator. The flare occurred on 2014 November 9. High-resolution slit-jaw 1330 A images from the Interface Region Imaging Spectrograph reveal four chromospheric flare ribbons that converge and form an X-shape. Flare brightening in the upper chromosphere spreads along the ribbons toward the center of the "X" (the X-point), and then spreads outward in a direction more perpendicular to the ribbons. These four ribbons are located in a quadrupolar magnetic field. Reconstruction of magnetic topology in the active region suggests the presence of a separator connecting to the X-point outlined by the ribbons. The inward motion of flare ribbons in the early stage therefore indicates 3D magnetic reconnection between two sets of non-coplanar loops that approach laterally, and reconnection proceeds downward along a section of vertical current sheet. Coronal loops are also observed by the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory confirming the reconnection morphology illustrated by ribbon evolution.
... Several methods have been developed over the years to identify separatrices and QSLs (see e.g. Longcope 2005;Démoulin 2006;Janvier et al. 2015, and references within). In the presence of twisted flux tubes, an analytical study of QSLs showed that they are expected to form a J-shaped structure delimiting the frontier between the flux rope and the surrounding field . ...
The standard model for eruptive flares has in the past few years been extended to 3D. It predicts typical J-shaped photospheric footprints of the coronal current layer, forming at similar locations as the Quasi-Separatrix Layers (QSLs). Such a morphology is also found for flare ribbons observed in the EUV band, as well as in non-linear force-free field (NLFFF) magnetic field extrapolations and models. We study the evolution of the photospheric traces of the current density and flare ribbons, both obtained with the SDO instruments. We investigate the photospheric current evolution during the 6 September 2011 X-class flare (SOL2011-09-06T22:20) from observational data of the magnetic field obtained with HMI. This evolution is compared with that of the flare ribbons observed in the EUV filters of the AIA. We also compare the observed electric current density and the flare ribbon morphology with that of the QSLs computed from the flux rope insertion method/NLFFF model. The NLFFF model shows the presence of a fan-spine configuration of overlying field lines, due to the presence of a parasitic polarity, embedding an elongated flux rope that appears in the observations as two parts of a filament. The QSLs, evolved via a magnetofrictional method, also show similar morphology and evolution as both the current ribbons and the EUV flare ribbons obtained at several times during the flare. For the first time, we propose a combined analysis of the photospheric traces of an eruptive flare, in a complex topology, with direct measurements of electric currents and QSLs from observational data and a magnetic field model. The results, obtained by two diff?erent and independent approaches, 1) confirm previous results of current increase during the impulsive phase of the flare, 2) show how NLFFF models can capture the essential physical signatures of flares even in a complex magnetic field topology.
... Furthermore, the structure of the magnetic field is usually characterized by the QSL, which denotes the place where the magnetic field line connectivity changes dramatically (Priest & Démoulin 1995;Démoulin et al. 1996aDémoulin et al. ,b, 1997Démoulin 2006;Mandrini et al. 1997;Titov et al. 2002). The QSL can be visualized by calculating the squashing factor, Q, which measures the gradient of the field line linkage (Titov et al. 2002). ...
... QSL is a place with very large gradient of the field line connectivity (Priest & Démoulin 1995;Démoulin et al. 1996aDémoulin et al. ,b, 1997Démoulin 2006;Mandrini et al. 1997;Titov et al. 2002), which is usually measured by the squashing factor, Q (Titov et al. 2002). Since field line connectivities of the MFR and the ambient field are quite different from each other, the value of Q can be very large at the interface between the MFR and the ambient field. ...
Magnetic flux rope (MFR) plays an important role in solar activities. A quantitative assessment of the topology of an MFR and its evolution is crucial for a better understanding of the relationship between the MFR and the associated activities. In this paper, we investigate the magnetic field of active region 12017 from 2014 March 28 to 29, where 12 flares were triggered by the intermittent eruptions of a filament (either successful or confined). Using the vector magnetic field data from the Helioseismic and Magnetic Imager on board the \textit{Solar Dynamics Observatory}, we calculate the magnetic energy and helicity injection in the active region, and extrapolate the 3D magnetic field with a nonlinear force-free field model. From the extrapolations, we find an MFR that is cospatial with the filament. We further determine the configuration of this MFR by a closed quasi-separatrix layer (QSL) around it. Then, we calculate the twist number and the magnetic helicity for the field lines composing the MFR. The results show that the closed QSL structure surrounding the MFR gets smaller as a consequence of the flare occurrence. We also find that the flares in our sample are mainly triggered by kink instability. Moreover, the twist number varies more sensitively than other parameters to the occurrence of flares.
... Portanto, todas as observações de AKR são feitas por satélites. Isso explica porque as emissões terrestres só foram descobertas no início da década de setenta, após o advento dos satélites destinados a observar a magnetosfera a grandes distâncias do planeta, aproximadamente vinte anos depois da descoberta das emissões similares de Júpiter (Jovian Decametric Radiation) [18]. As emissões jovianas possuem comprimento de onda que são da ordem de dezenas de metros, com frequências da ordem de dezenas de MHz, sendo suficientemente altas para ultrapassar o citado limite. ...
... Apesar de ser a mais intensa, a AKR nãoé aúnica emissão de ondas da magnetosfera. Devidoàs várias regiões distintas, caracterizadas por condições particulares de campo magnético e de plasmas, há várias outras emissões de ondas, tanto eletrostáticas quanto eletromagnéticas [18]. Porém, a origem de todas elasé basicamente a interação do vento solar com o campo geomagnético. ...
Several phenomena could be better studied and even disclosed after the development of the satellites and spacecrafts. Auroral kilometric radiation (AKR) is one of these phenomena. AKR was first detected only about forty years ago; its typical frequencies are too low to penetrate earthward across the ionosphere. This radiation is generated through wave-particle interactions, in the nightside region above the auroral ionosphere. It grows at the expense of free energy from the precipitating auroral electron beam. It is generated mainly in the extraordinary (X) mode, in the frequency range of 20-800 kHz, near the local electron cyclotron frequency. Nowadays, it is well known that AKR is intensified during magnetic substorms and has a good correlation with the AE magnetic index. However, recent studies showed that the radiation disappears in the initial and main phases of some magnetic storms, in spite of the large enhancement of the AE index and field aligned currents. The radiation activates strongly in the recovery phase. This behavior suggests that the field-aligned electric field, which accelerates precipitating electrons and drives field-aligned currents, is not formed in the initial and main phases of some magnetic storms. The purpose of this article is introduce readers to AKR and its features, making this important phenomenon best known among students and teachers of physics.
























