856 research outputs found
A stable auroral red arc over Europe
No full textUsing a new all-sky-imaging system, M Mendillo, C Barbieri, J Baumgardner, J Wroten, G Cremonese and G Umbriaco observed two distinctive types of aurora over London and western Europe on the night of 26-27 September 2011, including the first ground-based image of a stable auroral red arc over Europe
A stable auroral red arc over Europe
No full textUsing a new all-sky-imaging system, M Mendillo, C Barbieri, J Baumgardner, J Wroten, G Cremonese and G Umbriaco observed two distinctive types of aurora over London and western Europe on the night of 26-27 September 2011, including the first ground-based image of a stable auroral red arc over Europe. 2012 Royal Astronomical Society
Cabecar serratus Baumgardner & Ávila 2006, n. sp.
No full textCabecar serratus n. sp. Baumgardner and Ávila Mature Larva: Body length 3.5–4.0 mm; caudal filaments 2.0–3.0 mm. General color reddishbrown, frequently covered with extensive black maculations. Head: Reddish brown with variable black maculations; small genal projections present; tubercles absent; compound eyes small and widely separated; three ocelli present; antennae pale, approximately two times length of head capsule. Mouthparts: Labrum (Fig. 1): dorsally with filiform setae along lateral margin; two rows of acuminate setae recessed from anterior margin; ventrally with one longitudinal row of acuminate setae near midline, with interspersed filiform setae; anterior margin with filiform setae. Right mandible (Fig. 2): outer incisor three lobed, with robust setae at base; inner incisor two lobed; prostheca and molar region as in figure 2; scattered filiform setae on dorsal surface. Left mandible (Fig. 3): outer incisor four lobed, mostly fused; inner incisor two lobed, mostly fused; prostheca arising at base of inner incisor, with filiform setae projecting towards molar region; molar region as in figure 3; mandible with scattered filiform setae on dorsal surface. Hypopharynx (Fig. 4): lingua apically truncate; numerous filiform and acuminate setae present on anterior margin; superlinguae oval, with numerous filiform and acuminate setae along anterior and lateral margins. Maxilla (Fig. 5): palp elongate, twosegmented, with an elongate terminal seta; two subapical setae on inner apical margin; cluster of filiform setae on outer apical surface; filiform and acuminate setae along base of outer margin. Labium (Fig. 6): postmentum moderately developed, with regularlyspaced acuminate setae along lateral margins; ventrally with numerous robust setae most abundant near midline; prementum ventrally with numerous filiform setae; labial palp threesegmented with numerous filiform setae; glossae and paraglossae subequal, fused except distally, with smooth outer margins; glossae slightly recessed, rounded, and with robust setae; paraglossae with numerous filiform setae. Thorax: Reddish brown, often with extensive black maculations; pronotum with a pair of distinctive, sharp projections on anterior lateral margin (Fig. 7); mesonotum with a pair of small, rounded anterolateral tubercles (Fig. 7). Femur reddish brown with extensive dorsal black maculation; tibia reddish brown to black with pale maculation basally and apically; tarsus reddishbrown. Profemur (Fig. 8): dorsal surface with a transverse row of five or six chalazae, apical setae elongate with apices serrate; a second and slightly basal row of five or six chalazae also present, with apical setae elongate; two chalazae with apical setae elongate, with apices serrate, near center of femur; anterior and posterior margins of femur with numerous acuminate and elongate chalazae, becoming shorter towards apex of femur; filiform setae along basal anterior and posterior margins. Tibia and tarsus: margins with numerous acuminate and filiform setae; tibia with numerous, multibranched robust setae distally; tarsal claw with a single row of four or five denticles, basal denticle very small; remaining denticles similar in shape and size with equal spacing (Figure 9). Meso and metaleg femur (Fig. 10): dorsal surface with distinct median longitudinal row of four or five chalazae with apical setae elongate with apices serrate (Fig. 11); anterior and posterior margins with numerous acuminate chalazae, becoming shorter towards apex of femur. Tibia (Fig. 10): acuminate setae present along anterior and posterior margins; row of 1012 elongate setae present on dorsal surface; distally with numerous multibranched robust setae (visible under high magnification). Tarsus: four to six acuminate setae along inner margin. Claw (Fig. 12): with five or six denticles; apical denticles larger and more flattened than smaller, more sharply pointed, basal denticles. Abdomen: Reddish brown; some individuals with extensive black maculations; a median longitudinal pale line running length of terga; posterior margins of terga IX with numerous acuminate setae; filiform setae present along lateral margins of terga IX; posterolateral margins of abdominal segments VIIIX greatly expanded; segments VII and VIII, reaching approximately midpoint of next segment; segment IX projecting beyond posterior margin of segment X. Dorsal lamella of operculate gill (Fig. 13) on abdominal segment two subovate, reddish brown with extensive scattered black maculations; acuminate setae present along inner and apical margins; robust setae present along basal third of outer margin; gill formula (after Molineri, 2003): 2/3/4/4/2. Cerci with whorls of acuminate setae at each annulation. Male imago. Body length: 2.5–3.5 mm. Forewing length 2.5–3.5 mm. Hindwing absent. Cercus and median caudal filament length 11.0–12.0 mm. Head: brown with black maculation posterior to ocelli and lateral to compound eyes; vertex pale brown; compound eyes small, widely separated; diameter of one eye less than distance between eyes; lateral ocelli black at base, clear in distal onethird; median ocellus mostly clear; antenna pale; scape enlarged, remaining segments filiform. Thorax: tergum and sternum pale brown, contrasing strongly with the pale gray pleuron; tergum and pleuron with moderate to extensive black shading, most extensive on the pronotum.; membranous filaments on mesoscutellum (plumidium) absent. Femur: pale brown with very limited black maculation; foretibia purplish, dark brown at base; foretarsus purplish, threefourths length of foretibia; meso and metatibia pale reddish brown, dark brown at base; foreclaws similar and blunt; middle and hind claws dissimilar, one blunt, one pointed; hindfemur slightly shorter than hindtibia and handtarsus combined. Forewings (Fig. 14): translucent, margin opaque; costa, subcosta, and R1 purplish black for onehalf to threequarters their length, heavily pigmented purplishblack beyond margin of vein; vein ICu 1 joined basally with vein CuP; vein CuP present, not converging with vein AA; vein ICu 2 joined basally with ICu 1. Abdomen: tergites and sternites pale gray with moderate to extensive black overshading, mostly confined to medial region of tergites; cerci pale gray, bases with black stippling. Genitalia (Fig. 15): penes broad, fused for most of their distance, with shallow distomedial emargination; subgenital plate with moderately deep emargination; forceps three segmented, second segment with a basal swelling; segment one of forceps about as long as segments two and three combined. Female imago. Body length: 3.0–4.0 mm. Forewing length 3.0–3.5 mm. Hind wing absent. Cercus length 3.0–3.5 mm. Median caudal filament 2.5–3.0 mm. Head: as in male, except darker brown. Thorax: tergum and sternum dark redbrown with extensive overshadings of black dorsally and laterally; pleural region pale brown. Legs: dark reddishbrown with extensive black stippling; base of tibia with black ring. Forewings as in male, except with extensive black maculation at wing base. Abdomen: pale yellowishbrown, with extensive black stippling; subgential plate with posterior margin rounded; cercus and median pale gray; basal segments reddishbrown. Etymology: The specific epithet of this species is an adjective from the Latin word serratus (m), meaning serrated. It alludes to the serrated appearance of the margin of the femur. Discussion: The only significant variation observed in the larvae was the degree to which black maculations covered the body. Some larvae were entirely reddish brown with almost no black maculation, while other larvae were extensively covered with black. No morphological differences could be discerned between these two color variants, both of which were observed for both sexes. This variable coloration is likely a developmentallyinfluenced character, as is typical with many species of mayflies. A similar situation has also been observed in Leptohyphes zalope Traver, in which mature larvae may become very dark in appearance (Baumgardner and McCafferty 2000) as they near emergence to the adult stage. Distribution and Biology: Cabecar serratus is currently known only from lowland costal regions of both the Atlantic and Pacific slopes of Nicaragua, Costa Rica, and Panamá. Larvae were collected from leaf packs and the surface of rocks and woody debris found in the slower regions of small streams. Their bodies were frequently covered by thick periphyton biofilm. HOLOTYPE: Mature Female Larva — COSTA RICA: Limón Province, unnamed creek at Hwy 32, ca. 3 km W Pocora (10º10'38"N, 83º37'03"W, elev. 110 m), 10.vi.2001, DE Baumgardner (DB 0129), deposited in the Texas A & M University Insect Museum, College Station, Texas. PARATYPES: Same data as holotype, 1 mature female larva (FAMU); COSTA RICA: Puntarenas.: Río Barú at Barú, ca. 5 km NE Dominical, 22.vi.2001, 3L, 1 slide (#DB 02i2002), DEB (DB 0149) (TAMU); Río Balsar at Hwy 34, ca. 8 km NW Palmar Norte (08º59'05"N, 83º31'07"W; elev. 65m), 22.vi.2001, 1L, DEB (DB 0153) (PERC). Golfito, Quebrada Km. 20, 21.iii.2005, 1♂ subimago (reared), S. Avila (TAMU). Río Claro, Quebrada Chiricanos, puente de C.I.A., 12.iii.2005, 1♂ (reared), 1♂ (slide #DB 05x2101), 1♀, S. Ávila (TAMU). Golfito, Río Claro, Golfito, Queb. Lagarto, 21.iii.2005, 2♂, 3♀, S. Ávila (TAMU). Limón: Río Suzrez at Hwy 36, ca. 17 Km NW Bribri (09º43'36"N, 82º50'21"W; elev. 20 m), 11.vi.2001, 1L, DEB (DB 0130) (INBio). NICARAGUA: Granada: unnamed creek at Domitila Field Station, ca. 30 km S Granada (11º42'09"N, 85º57'06"W; elev. 80 m), 1318.vi.2004, DEB (DB 0441), 12L, 1 slide (#DB04x3001) (8L TAMU, 2L each FAMU, PERC). Material Excluded From Type Series: NICARAGUA: Río San Juan: Bartola Field Station, Río San Juan, ca. 3 km SE El Castillo (10º58'22"N, 84º20'24"W; elev. 50 m), 1924.vi.2004, 1L (immature), DEB (DB 0443) (TAMU). PANAMÁ: Panamá, Capira, Río Capira, tierras bajas, 15iv1995, Coll. J. Coronado, 1L (TAMU).Published as part of Baumgardner, David E. & Ávila, Socorro, 2006, Cabecar serratus, a new genus and species of leptohyphid mayfly from Central America, and description of the imaginal stages of Tricorythodes sordidus Allen (Ephemeroptera: Leptohyphidae), pp. 47-59 in Zootaxa 1187 (1) on pages 49-54, DOI: 10.11646/zootaxa.1187.1.3, http://zenodo.org/record/506422
Overdosing and Attempted Suicide among Youth in an Affluent Suburban Community
No full text Dr. Tobias, Associate Professor of Counsellor Education at the University of Detroit and Director of the Community Youth Relations Bureau in Bloomfield Township, Michigan, and Marilyn Baumgardner, student assistant, discuss teenage overdosing and suicidal attempts in this affluent community during the past few years. </jats:p
Imaging Space Weather Over Europe from a Single Site
No full textWe have recently installed a low-light-level, all-sky-imager (ASI) at the astronomical observatory in Asiago, Italy (45.8 N, 11.5 E, 41 N geomagnetic). The field-of-view for such a system can yield reliable observations from zenith down to about five degrees elevation angle. Atmospheric emissions arise from different altitudes and thus the spatial region observed by an ASI depends on the specific wavelength (and process) involved. For 6300 A emissions from atomic oxygen, diffuse aurora occur at ~200 km, ambient airglow at ~300 km and so-called Stable Auroral Red (SAR) arcs at ~400 km. From the Asiago site, the FOV at 400 km spans latitudes extending from southern Scandanavia to Northern Africa. For a magnetic latitude of 50 N, longitudes observed to the north extend from Ireland to Belarus. For a magnetic latitude of 30 N, longitudes to the south can be observed from Spain to Turkey. The SAR arc that occurred during the geomagnetic storm 26-27 September 2011 was, we think, the first-ever such event imaged from the ground in Europe. The SAR arc’s location throughout the night maps to the inner magnetosphere where the plasmapause and inner edge of the ring current coincide. The spatial-temporal positions of these features determine the lowest latitudes of magnetosphere-ionospheric energy input during space weather events. We show that an all-sky-imager can thus be used to provide real-time information of this boundary over most of Europe—and thus the low-latitude limit of the radiowave scintillations associated with SAR arcs. Moreover, such information can be used for retrospective validations of global models that predict the latitude extent of space weather effects
First Conjugate Observations of Medium-Scale Traveling Ionospheric Disturbances (MSTIDs) in the Europe-Africa Longitude Sector
No full textAll-sky imagers located in Asiago, Italy (45.87oN, 11.53oE; 40.7o magnetic latitude) and Sutherland, South Africa (32.37oS, 20.81oE; −40.7o magnetic latitude) are used to study magnetically conjugate medium scale traveling ionospheric disturbances (MSTIDs). We present initial results from the first year of joint Asiago-Sutherland data sets from July 2016 to June 2017. The 630.0-nm airglow perturbations showing different kinds of waves were frequently observed. Some of these wave events resemble MSTIDs propagating south-westward in Asiago, typical direction observed at other longitude sectors in the northern hemisphere. They are mostly observed as single bands propagating through the field of view of the all-sky imagers. We select and analyze five cases of magnetically conjugate bands associated with MSTIDs. The bands observed at Sutherland move mainly westward, noticeably different from the north-west direction of propagation of MSTIDs observed in the southern hemisphere. We compare the MSTIDs propagation speeds and find that three cases show larger values at Sutherland. When we compare the zonal speeds all the cases show larger values at Sutherland. On average, the propagation speed at Sutherland is 20% larger and the zonal speed is ~35% larger. The westward motion at Sutherland is explained by taking onto account how its magnetic declination (~24oW) affects the orientation of the bands. The larger speed at Sutherland is due to the weaker Earth's magnetic field in the southern hemisphere and the particular configuration of the magnetic field lines in this longitude sector.All-sky imagers located in Asiago, Italy (45.87 o N, 11.53 o E; 40.7 o magnetic latitude) and Sutherland, South Africa (32.37 o S, 20.81 o E; −40.7 o magnetic latitude) are used to study magnetically conjugate medium scale traveling ionospheric disturbances (MSTIDs). We present initial results from the first year of joint Asiago-Sutherland data sets from July 2016 to June 2017. The 630.0-nm airglow perturbations showing different kinds of waves were frequently observed. Some of these wave events resemble MSTIDs propagating south-westward in Asiago, typical direction observed at other longitude sectors in the northern hemisphere. They are mostly observed as single bands propagating through the field of view of the all-sky imagers. We select and analyze five cases of magnetically conjugate bands associated with MSTIDs. The bands observed at Sutherland move mainly westward, noticeably different from the north-west direction of propagation of MSTIDs observed in the southern hemisphere. We compare the MSTIDs propagation speeds and find that three cases show larger values at Sutherland. When we compare the zonal speeds all the cases show larger values at Sutherland. On average, the propagation speed at Sutherland is 20% larger and the zonal speed is ~35% larger. The westward motion at Sutherland is explained by taking onto account how its magnetic declination (~24 o W) affects the orientation of the bands. The larger speed at Sutherland is due to the weaker Earth's magnetic field in the southern hemisphere and the particular configuration of the magnetic field lines in this longitude sector
Imaging space weather over Europe
No full text[1] We describe the introduction of the first all-sky imaging system for low-light-level optical observations of the disturbed ionosphere over mid-latitude Europe. Using 6300 angstrom auroral emissions that come from the 200-400 km altitude range, we demonstrate that sub-visual optical patterns spanning the European continent can be obtained from a single site in Italy. Pilot observations during the 26-27 September 2011 geomagnetic storm show that the diffuse aurora's low latitude boundary can be used to find where the poleward wall of the ionospheric trough is located. This relates directly to regions of radiowave disruptions caused by the precipitation of energetic particles from the magnetospheric plasma sheet that move to lower latitudes during space weather events. Images of stable auroral red (SAR) arcs can be used to track the magnetospheric ring current and plasmapause location, a second region of radiowave interference. Comparisons with ground-based and satellite observations of the ionosphere during the same storm demonstrate how ASI images reveal the lowest energy components of magnetospheric input to the ionosphere-thermosphere system. Such observations can be used, potentially, for both now-casting of storm effects spanning Europe, and for retrospective validation of existing models of space weather impacts at sub-auroral locations. Citation: Baumgardner, J., et al. (2013), Imaging space weather over Europe, Space Weather, 11, 69-78, doi:10.1002/swe.20027
Imaging Space Weather Over Europe from a Single Site
No full textWe have recently installed a low-light-level, all-sky-imager (ASI) at the astronomical observatory in Asiago, Italy (45.8 N, 11.5 E, 41 N geomagnetic). The field-of-view for such a system can yield reliable observations from zenith down to about five degrees elevation angle. Atmospheric emissions arise from different altitudes and thus the spatial region observed by an ASI depends on the specific wavelength (and process) involved. For 6300 A emissions from atomic oxygen, diffuse aurora occur at ~200 km, ambient airglow at ~300 km and so-called Stable Auroral Red (SAR) arcs at ~400 km. From the Asiago site, the FOV at 400 km spans latitudes extending from southern Scandanavia to Northern Africa. For a magnetic latitude of 50 N, longitudes observed to the north extend from Ireland to Belarus. For a magnetic latitude of 30 N, longitudes to the south can be observed from Spain to Turkey. The SAR arc that occurred during the geomagnetic storm 26-27 September 2011 was, we think, the first-ever such event imaged from the ground in Europe. The SAR arc’s location throughout the night maps to the inner magnetosphere where the plasmapause and inner edge of the ring current coincide. The spatial-temporal positions of these features determine the lowest latitudes of magnetosphere-ionospheric energy input during space weather events. We show that an all-sky-imager can thus be used to provide real-time information of this boundary over most of Europe—and thus the low-latitude limit of the radiowave scintillations associated with SAR arcs. Moreover, such information can be used for retrospective validations of global models that predict the latitude extent of space weather effects
High resolution measurements and modeling of auroral hydrogen emission line profiles
No full textMeasurements in the visible wavelength range at
high spectral resolution (1.3 A° ) have been made at Longyearbyen,
Svalbard (15.8 E,78.2 N) during an interval of intense
proton precipitation. The shape and Doppler shift of hydrogen
Balmer beta line profiles have been compared with
model line profiles, using as input ion energy spectra from
almost coincident passes of the FAST and DMSP spacecraft.
The comparison shows that the simulation contains the important
physical processes that produce the profiles, and confirms
that measured changes in the shape and peak wavelength
of the hydrogen profiles are the result of changing
energy input. This combination of high resolution measurements
with modeling provides a method of estimating the
incoming energy and changes in flux of precipitating protons
over Svalbard, for given energy and pitch-angle distributions.
Whereas for electron precipitation, information on the incident
particles is derived from brightness and brightness ratios
which require at least two spectral windows, for proton precipitation
the Doppler profile of resulting hydrogen emission
is directly related to the energy and energy flux of the incident
energetic protons and can be used to gather information
about the source region. As well as the expected Doppler
shift to shorter wavelengths, the measured profiles have a significant
red-shifted component, the result of upward flowing
emitting hydrogen atoms
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