cometadata/datacite-rtg-text-other-reclassification-records huggingface dataset:
Double flows anchored in a Kerr black hole horizon. I. Meridionally self-similar MHD models with loading terms
Creators: name: Chantry, L.
name: Cayatte, V.
name: Sauty, C.
name: Vlahakis, N.
name: Tsinganos, K.
Publisher: name: arXiv
Year: 2022
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: Recent observations of supermassive black holes have brought us new information on their magnetospheres. In this study we attempt a theoretical modelling of the coupling of black holes with their jets and discs, via three innovations. First, we propose a semi-analytical MHD description of a steady relativistic inflow-outflow structure characteristic to the extraction of the hole rotational energy. The mass-loading is ensured in a thin layer, the stagnation surface, by a two-photon pair production originating to a gamma-ray emission from the surrounding disc. The double flow is described near the polar axis by an axisymmetric meridionally self-similar MHD model. Second, the inflow and outflow solutions are crossing the MHD critical points and are matched at the stagnation surface. Knowledge of the MHD field on the horizon give us the angular momentum and energy extracted from the black hole. Finally, we illustrate the model with three specific examples of double-flow solutions by varying the energetic interaction between the MHD field and the rotating black hole. When the isorotation frequency is half of the black hole one, the extracted Poynting flux is comparable to the one obtained using the force-free assumption. In two of the presented solutions, the Penrose process dominates at large colatitudes, while the third is Poynting flux dominated at mid colatitudes. Mass injection rate estimations, from disk luminosity and inner radius, give an upper limit just above the values obtained for two solutions. This model is pertinent to describe the flows near the polar axis where pair production is more efficient.
description: 22 page
Observing the Reionization : Effect of Calibration and Position Errors on Realistic Observation Conditions
Creators: name: Mazumder, Aishrila
name: Datta, Abhirup
name: Chakraborty, Arnab
name: Majumdar, Suman
Publisher: name: arXiv
Year: 2022
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: Instrumentation and Methods for Astrophysics (astro-ph.IM)
subject: FOS: Physical sciences

description: Observation of the redshifted 21-cm signal from Cosmic Dawn and Epoch of Reionization is a challenging endeavor in observational cosmology. Presence of orders of magnitude brighter astrophysical foregrounds and various instrumental systematics increases the complexity of these observations. This work presents an end-to-end pipeline dealing with synthetic interferometric data of sensitive radio observations . The mock sky model includes the redshifted 21-cm signal and astrophysical foregrounds. The effects of calibration error and position error in the extraction of the redshifted 21-cm power spectrum has been simulated. The effect of the errors in the image plane detection of the cosmological signal has also been studied. A comparative analysis for array configurations like the SKA1-Low, MWA and HERA has been demonstrated. The calibration error tolerance of the arrays, under some assumptions about the nature of the systematic components, is optimally found to be $\sim 0.01\%$ for the detection of the signal. For position errors, an offset of $\gtrapprox 5\arcsec$ makes the residual foregrounds obscure the target signal. These simulations also imply that in the SKA-1 Low performs marginally better than the others in the image domain, while the same is true for MWA in the power spectrum domain. This is one of the first studies that compares performance of various radio telescopes operating under similar observing conditions towards detecting the cosmological signal. This end-to-end pipeline can also be extended to study effects of chromatic primary beam, radio frequency inferences, foregrounds with spectral features, etc.
description: 19 pages, 21 figures, Accepted for publication in MNRAS
HST/WFC3 H$α$ Direct-Imaging Detection of a Point-like Source in the Disk Cavity of AB Aur
Creators: name: Zhou, Yifan
name: Sanghi, Aniket
name: Bowler, Brendan P.
name: Wu, Ya-Lin
name: Close, Laird M.
name: Long, Feng
name: Ward-Duong, Kimberly
name: Zhu, Zhaohuan
name: Kraus, Adam L.
name: Follette, Katherine B.
name: Bae, Jaehan
Publisher: name: arXiv
Year: 2022
Subjects: subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences

description: Accreting protoplanets enable the direct characterization of planet formation. As part of a high-contrast imaging search for accreting planets with the Hubble Space Telescope (HST) Wide Field Camera 3, we present H$α$ images of AB Aurigae (AB Aur), a Herbig Ae/Be star harboring a transition disk. The data were collected in two epochs of direct-imaging observations using the F656N narrow-band filter. After subtracting the point spread function of the primary star, we identify a point-like source located at a P.A. of $182.5^{\circ}\pm1.4^{\circ}$ and a separation of $600\pm22$~mas relative to the host star. The position is consistent with the recently identified protoplanet candidate AB Aur b. The source is visible in two individual epochs separated by ${\sim}50$ days and the H$α$ intensities in the two epochs agree. The H$α$ flux density is $F_ν=1.5\pm0.4$~mJy, $3.2\pm0.9$ times of the optical continuum determined by published HST/STIS photometry. In comparison to PDS 70 b and c, the H$α$ excess emission is weak. The central star is accreting and the stellar H$α$ emission has a similar line-to-continuum ratio as seen in AB Aur b. We conclude that both planetary accretion and scattered stellar light are possible sources of the H$α$ emission, and the H$α$ detection alone does not validate AB Aur b as an accreting protoplanet. Disentangling the origin of the emission will be crucial for probing planet formation in the AB Aur disk.
description: Accepted for publication in ApJL
Formation of Quiescent Prominence Magnetic Field by Supergranulations
Creators: name: Liu, Qingjun
name: Xia, Chun
Publisher: name: arXiv
Year: 2022
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences

description: To understand the formation of quiescent solar prominences, the origin of their magnetic field structures, i.e., magnetic flux ropes (MFRs), must be revealed. We use three-dimensional magnetofriction simulations in a spherical subdomain to investigate the role of typical supergranular motions in the long-term formation of a prominence magnetic field. Time-dependant horizontal supergranular motions with and without the effect of Coriolis force are simulated on the solar surface via Voronoi tessellation. The vortical motions by the Coriolis effect at boundaries of supergranules inject magnetic helicity into the corona. The helicity is transferred and accumulated along the polarity inversion line (PIL) as strongly sheared magnetic field via helicity condensation. The diverging motions of supergranules converge opposite magnetic polarities at the PIL and drive the magnetic reconnection between footpoints of the sheared magnetic arcades to form an MFR. The magnetic network, negative-helicity MFR in the northern hemisphere, and fragmented-to-continuous formation process of magnetic dip regions are in agreement with observations. Although diverging supergranulations, differential rotation, and meridional flows are included, the simulation without the Coriolis effect can not produce an MFR or sheared arcades to host a prominence. Therefore Coriolis force is a key factor for helicity injection and the formation of magnetic structures of quiescent solar prominences.
description: 5 figures
Theoretically Modelling Photoionized Regions with Fractal Geometry in Three Dimensions
Creators: name: Jin, Yifei
name: Kewley, Lisa J.
name: Sutherland, Ralph S.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: We create a photoionization model embedded in the turbulent ISM by using the state-of-the-art Messenger Monte-Carlo MAPPINGS~V code (M$^3$) in conjunction with the CMFGEN stellar atmosphere model. We show that the turbulent ISM causes the inhomogeneity of electron temperature and density within the nebula. The fluctuation in the turbulent ISM creates complex ionization structures seen in nearby nebulae. The inhomogeneous density distribution within the nebula creates a significant scatter on the spatially-resolved standard optical diagnostic diagrams, which cannot be represented by the spherical constant density photoionization model. We analyze the dependence of different optical emission lines on the complexity of nebular geometry, finding that the emission-lines residing on the nebular boundary are highly sensitive to the complexity of nebular geometry, while the emission-lines produced throughout the nebula are sensitive to the density distribution of the ISM within the nebula. Our fractal photoionization model demonstrates that a complex nebular geometry is required for accurate modeling of HII regions and emission-line galaxies, especially for the high-redshift galaxies, where the ISM is highly turbulent based on the increasing observational evidence.
description: Accepted for Publication in ApJL
First report of a solar energetic particle event observed by China's Tianwen-1 mission in transit to Mars
Creators: name: Fu, Shuai
name: Ding, Zheyi
name: Zhang, Yongjie
name: Zhang, Xiaoping
name: Li, Cunhui
name: Li, Gang
name: Tang, Shuwen
name: Zhang, Haiyan
name: Xu, Yi
name: Wang, Yuming
name: Guo, Jingnan
name: Zhao, Lingling
name: Wang, Yi
name: Hu, Xiangyu
name: Luo, Pengwei
name: Sun, Zhiyu
name: Yu, Yuhong
name: Xie, Lianghai
Publisher: name: arXiv
Year: 2022
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: Space Physics (physics.space-ph)
subject: FOS: Physical sciences

description: Solar energetic particles (SEPs) associated with flares and/or coronal mass ejection (CME)-driven shocks can impose acute radiation hazards to space explorations. To measure energetic particles in near-Mars space, the Mars Energetic Particle Analyzer (MEPA) instrument onboard China's Tianwen-1 (TW-1) mission was designed. Here, we report the first MEPA measurements of the widespread SEP event occurring on 29 November 2020 when TW-1 was in transit to Mars. This event occurred when TW-1 and Earth were magnetically well connected, known as the Hohmann-Parker effect, thus offering a rare opportunity to understand the underlying particle acceleration and transport process. Measurements from TW-1 and near-Earth spacecraft show similar double-power-law spectra and a radial dependence of the SEP peak intensities. Moreover, the decay phases of the time-intensity profiles at different locations clearly show the reservoir effect. We conclude that the double-power-law spectrum is likely generated at the acceleration site, and that a small but finite cross-field diffusion is crucial to understand the formation of the SEP reservoir phenomenon. These results provide insight into particle acceleration and transport associated with CME-driven shocks, which may contribute to the improvement of relevant physical models.
description: This manuscript has been accepted for publication in The Astrophysical Journal Letters
Faculae cancel out on the surfaces of active Suns
Creators: name: Nèmec, N. -E.
name: Shapiro, A. I.
name: Işık, E.
name: Sowmya, K.
name: Solanki, S. K.
name: Krivova, N. A.
name: Cameron, R. H.
name: Gizon, L.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: FOS: Physical sciences

description: Surfaces of the Sun and other cool stars are filled with magnetic fields, which are either seen as dark compact spots or more diffuse bright structures like faculae. Both hamper detection and characterisation of exoplanets, affecting stellar brightness and spectra, as well as transmission spectra. However, the expected facular and spot signals in stellar data are quite different, for instance they have distinct temporal and spectral profiles. Consequently, corrections of stellar data for magnetic activity can greatly benefit from the insight on whether the stellar signal is dominated by spots or faculae. Here, we utilise a surface flux transport model (SFTM) to show that more effective cancellation of diffuse magnetic flux associated with faculae leads to spot area coverages increasing faster with stellar magnetic activity than that by faculae. Our calculations explain the observed dependence between solar spot and facular area coverages and allow its extension to stars more active than the Sun. This extension enables anticipating the properties of stellar signal and its more reliable mitigation, leading to a more accurate characterisation of exoplanets and their atmospheres.
description: 10 pages, 6 Figures, accepted for publication in ApJL
On the accretion of a new group of galaxies onto Virgo: II. The effect of pre-processing on the stellar population content of dEs
Creators: name: Bidaran, Bahar
name: La Barbera, Francesco
name: Pasquali, Anna
name: Peletier, Reynier
name: van de Ven, Glenn
name: Grebel, Eva K.
name: Falcón-Barroso, Jesus
name: Sybilska, Agnieszka
name: Gadotti, Dimitri A.
name: Coccato, Lodovico
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: Using MUSE spectra, we investigate how pre-processing and accretion onto a galaxy cluster affect the integrated stellar population properties of dwarf early-type galaxies (dEs). We analyze a sample of nine dEs with stellar masses of $\rm \sim 10^9 \, M_\odot$, which were accreted ($\sim$ 2-3 Gyr ago) onto the Virgo cluster as members of a massive galaxy group. We derive their stellar population properties, namely age, metallicity ([M/H]), and the abundance ratio of $α$ elements ([$α$/Fe]), by fitting observed spectral indices with a robust, iterative procedure, and infer their star formation history (SFH) by means of full spectral fitting. We find that these nine dEs are more metal-poor (at the 2-3$σ$ level) and significantly more $α$-enhanced than dEs in the Virgo and Coma clusters with similar stellar mass, cluster-centric distance, and infall time. Moreover, for six dEs, we find evidence for a recent episode of star formation during or right after the time of accretion onto Virgo. We interpret the high [$α$/Fe] of our sample of dEs as the result of the previous exposure of these galaxies to an environment hostile to star formation, and/or the putative short burst of star formation they underwent after infall into Virgo. Our results suggest that the stellar population properties of low-mass galaxies may be the result of the combined effect of pre-processing in galaxy groups and environmental processes (such as ram-pressure triggering star formation) acting during the early phases of accretion onto a cluster.
description: 17 pages, 10 figures, Accepted for publication in MNRAS
Becoming in 5 parts.mp3
Creators: name: ROBINSON, PHILLIPA
Publisher: name: University of Melbourne
Year: 2021
Subjects: Other education not elsewhere classified
Secondary education
Teacher education and professional development of educators
Specialist studies in education not elsewhere classified
Creative arts, media and communication curriculum and pedagogy
Performing arts not elsewhere classified

description: A musical accompaniment to my a/r/tographic thesis.
Impulsively Generated Kink Wave Trains in Solar Coronal Slabs
Creators: name: Guo, Mingzhe
name: Li, Bo
name: Van Doorsselaere, Tom
name: Shi, Mijie
Publisher: name: arXiv
Year: 2022
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences

description: We numerically follow the response of density-enhanced slabs to impulsive, localized, transverse velocity perturbations by working in the framework of ideal magnetohydrodynamics (MHD). Both linear and nonlinear regimes are addressed. Kink wave trains are seen to develop along the examined slabs, sharing the characteristics that more oscillatory patterns emerge with time and that the apparent wavelength increases with distance at a given instant. Two features nonetheless arise due to nonlinearity, one being a density cavity close to the exciter and the other being the appearance of shocks both outside and inside the nominal slab. These features may be relevant for understanding the interaction between magnetic structures and such explosive events as coronal mass ejections. Our numerical findings on kink wave trains in solar coronal slabs are discussed in connection with typical measurements of streamer waves.
description: 10 pages, 8 figures, accepted for publication in MNRAS
Can we reveal the core-chemical composition of ultra-massive white dwarfs through their magnetic fields?
Creators: name: Camisassa, Maria E.
name: Raddi, Roberto
name: Althaus, Leandro G.
name: Isern, Jordi
name: Rebassa-Mansergas, Alberto
name: Torres, Santiago
name: Corsico, Alejandro H.
name: Korre, Lydia
Publisher: name: arXiv
Year: 2022
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: Ultra-massive white dwarfs ($ 1.05 \rm M_\odot \lesssim M_{WD}$) are particularly interesting objects that allow us to study extreme astrophysical phenomena such as type Ia supernovae explosions and merger events. Traditionally, ultra-massive white dwarfs are thought to harbour oxygen-neon (ONe) cores. However, recent theoretical studies and new observations suggest that some ultra-massive white dwarfs could harbour carbon-oxygen (CO) cores. Although several studies have attempted to elucidate the core composition of ultra-massive white dwarfs, to date, it has not been possible to distinguish them through their observed properties. Here, we present a new method for revealing the core-chemical composition in ultra-massive white dwarfs that is based on the study of magnetic fields generated by convective mixing induced by the crystallization process. ONe white dwarfs crystallize at higher luminosities than their CO counterparts. Therefore, the study of magnetic ultra-massive white dwarfs in the particular domain where ONe cores have reached the crystallization conditions but CO cores have not, may provide valuable support to their ONe core-chemical composition, since ONe white dwarfs would display signs of magnetic fields and CO would not. We apply our method to eight white dwarfs with magnetic field measurements and we suggest that these stars are candidate ONe white dwarfs.
description: Accepted for publication in MNRAS Letters
AfGT 2021 Annual Report.pdf
Creators: name: KEAMY, RON
name: CLINTON, JANET
name: TAN, KATINA YEE SHAN
Publisher: name: University of Melbourne
Year: 2021
Subjects: Other education not elsewhere classified
Teacher education and professional development of educators

description: Assessment for Graduate Teaching Report 2021: Prepared for the Assessment for Graduate Teaching (AfGT) ConsortiumCollaborators & Licensees
The fall of CSS100217: a tidal disruption-induced low state in an apparently hostless active galactic nucleus
Creators: name: Cannizzaro, G.
name: Levan, A. J.
name: van Velzen, S.
name: Brown, G.
Publisher: name: arXiv
Year: 2022
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: CSS100217 was a nuclear, rapid and luminous flare in a Narrow-Line Seyfert 1 galaxy, whose initial interpretation as a supernova is now debated between variability of the active galactic nucleus (AGN) or a tidal disruption event (TDE). In this paper, we present and discuss new evidence in favour of a TDE or extreme flaring episode scenario. After the decay of the flare, the galaxy entered a long-term low luminosity state, 0.4 magnitudes lower than the pre-outburst emission in the V band. We attribute this to the creation of a cavity in the accretion disk after the tidal disruption of a star in a retrograde orbit with respect to the accretion disk rotation, making a TDE our favoured interpretation of the flare. We also show how the host galaxy shows a point-like, compact profile, no evidence for an extended component and a relatively low mass, unlike what expected from an AGN host galaxy at z=0.147. A compact host galaxy may result in an increased TDE rate, strengthening our interpretation of the event.
description: 11 pages, 4 figures, accepted for publication on MNRAS
Testechiniscus meridionalis
Creators: name: Gąsiorek, Piotr
name: Stec, Daniel
name: Zawierucha, Krzysztof
name: Kristensen, Reinhardt Møbjerg
name: Michalczyk, Łukasz
Publisher: name: Zenodo
Year: 2018
Subjects: Biodiversity
Taxonomy
Animalia
Tardigrada
Heterotardigrada
Echiniscoidea
Echiniscidae
Testechiniscus
Testechiniscus meridionalis

description: Autapomorphies of Testechiniscus meridionalis (Murray, 1906) and T. macronyx (Richters, 1907)
(measurements and statistics of juveniles and adult specimens of both sexes of T. meridionalis in Tables 10–12)
Both species assigned to the genus Testechiniscus by Kristensen (1987) and McInnes (1994a), respectively, exhibit unique phenotypic traits. Given that works on their systematic position are in progress (McInnes, personal communication), we do not designate them as new genera, but, instead, we present their autapomorphies, which exclude their affiliation within the revised Testechiniscus. Both species have brown lipoid or red eyes and are dioecious whereas Testechiniscus s.s. exhibits black crystalline eyes and parthenogenetic reproduction (although the presence of males was suggested in T. laterculus by Kathman & Dastych (1990)).
Moreover, T. meridionalis resembles Testechiniscus s.s. in having eight rows of ventral plates, however it differs from Testechiniscus s.s. by: a smaller body size, i.e. with adults not exceeding 200 µm (compare Figs 1A–B, 6A–B, 10A–C and 12A–B, see Tables 10–11), whereas adults of Testechiniscus spp. are typically 300–450 µm long; smaller ventral plates (Figs 12C–D) with minute cuticular pillars that are more like in the Bryodelphax weglarskae group (see Dastych 1984, Kaczmarek et al. 2012) rather than in Testechiniscus spp.; the dorsal sculpture consisting solely of granules (Fig. 14E) and never polygonal pores typical for Testechiniscus (e.g. Fig. 14A); evident sexual dimorphism, i.e. cephalic papillae and primary clavae are significantly longer in males than in females (one-tailed Welch t -test for: cephalic papillae: t 3=4.07, p=0.013, and primary clavae: t 3=4.14, p=0.013, compare also Figs 12A, D, arrowheads).
Finally, T. macronyx differs from the revised Testechiniscus by: a smaller body size (i.e. below 200 µm); the presence of only lateral, exceptionally long cirri A (Fig. 13A); nine (instead of eight) rows of small ventral plates (configuration IX:2-5-5-2-4-4-4-1-2, Fig. 13B); dorsal sculpture in the form of an irregular reticulum/pseudopores (see McInnes 1994a), that look like dark margins of minute bright depressions on the cuticle surface (Fig. 14F); and by considerably longer claws, curved slightly only in their terminal parts.
description: Published as part of Gąsiorek, Piotr, Stec, Daniel, Zawierucha, Krzysztof, Kristensen, Reinhardt Møbjerg & Michalczyk, Łukasz, 2018, Revision of Testechiniscus Kristensen, 1987 (Heterotardigrada: Echiniscidae) refutes the polar-temperate distribution of the genus, pp. 261-297 in Zootaxa 4472 (2) on page 285, DOI: 10.11646/zootaxa.4472.2.3, http://zenodo.org/record/1440175
Achillea ageratum L.
Creators: name: Info Flora
Publisher: name: Zenodo
Year: 2021
Subjects: Biodiversity
Taxonomy
Plantae
Tracheophyta
Magnoliopsida
Asterales
Asteraceae
Achillea
Achillea ageratum

description: Achillea ageratum L.
Balsam-Schafgarbe
Art ISFS: 950 Checklist: 1000170 Asteraceae Achillea Achillea ageratum L.
Bestimmungsschlüssel
ZusammenfassungKEINE ANGABE
Ökologie
Lebensraum Lebensraumnach Delarze & al. 2015
KEINE ANGABE
Ökologische Zeigerwerte nach Landolt & al. (2010)
BodenfaktorenKlimafaktorenSalztoleranzFeuchtezahl F--Lichtzahl L--Salzzeichen--Reaktionszahl R--Temperaturzahl T--Nährstoffzahl N--Kontinentalitätszahl K--
Nomenklatur
Gültiger Name (Checklist 2017):Achillea ageratumL.
Volksname Deutscher Name: Balsam-Schafgarbe Nom français: Achillée à feuilles d'agératum Nome italiano: Millefoglio agerato
Übereinstimmung mit anderen Referenzwerken
RelationNomReferenzwerkeNo=Achillea ageratum L.Checklist 2017950
= Taxon stimmt mit akzeptiertem Taxon überein (Checklist 2017)  Taxon enthält (neben anderen) auch das akzeptierte Taxon (Checklist 2017)
Kommentare aus der Checklist 2017 Neues Taxon: Gegenüber SISF-2 neu aufgenommener Neophyt. Checklist
Status Indigenat: Neophyt: nach der Entdeckung von Amerika in der Region aufgetreten (nach 1500)
Liste der gefährdeten Pflanzen IUCN(nach Walter & Gillett 1997): Nein
description: Published as part of Info Flora, 2021,
OpenOrgs: bridging registries of research organizations. Supporting disambiguation and improving the quality of data
Creators: name: Pavone, Gina
name: Atzori, Claudio
Publisher: name: Zenodo
Year: 2021
Subjects: Open Science, OpenOrgs, OpenAIRE, discoverability, disambiguation,

description: This presentation was given for OpenAIRE Tech Clinic webinar on 21 June 2021, focusing on the OpenOrgs tool. Unambiguously identifying organizations involved in the research work may not be a trivial task. Their names can be derived from various data sources, each of which often contains a different version of the organization's name (full legal name, short or alternative names, acronym, and so on) and different metadata fields. In OpenOrgs, data curators can enrich the metadata description of organizations and resolve the ambiguity of duplicates detected with an automated process by stating whether two or more entities correspond or not to the same organization. With these tasks, OpenOrgs users can compensate for the lack of information available and improve the organizations' discoverability.
SDSS-IV MaNGA: Global Properties of Kinematically Misaligned Galaxies
Creators: name: Zhou, Yuren
name: Chen, Yanmei
name: Shi, Yong
name: Bizyaev, Dmitry
name: Guo, Hong
name: Bao, Min
name: Xu, Haitong
name: Yu, Xiaoling
name: Brownstein, Joel R.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: We select 456 gas-star kinematically misaligned galaxies from the internal Product Launch-10 of MaNGA survey, including 74 star-forming (SF), 136 green-valley (GV) and 206 quiescent (QS) galaxies. We find that the distributions of difference between gas and star position angles for galaxies have three local peaks at $\sim0^{\circ}$, $90^{\circ}$, $180^{\circ}$. The fraction of misaligned galaxies peaks at $\log(M_*/M_{\odot})\sim10.5$ and declines to both low and high mass end. This fraction decreases monotonically with increasing SFR and sSFR. We compare the global parameters including gas kinematic asymmetry $V_{\mathrm{asym}}$, HI detection rate and mass fraction of molecular gas, effective radius $R_e$, Sérsic index $n$ as well as spin parameter $λ_{R_e}$ between misaligned galaxies and their control samples. We find that the misaligned galaxies have lower HI detection rate and molecular gas mass fraction, smaller size, higher Sérsic index and lower spin parameters than their control samples. The SF and GV misaligned galaxies are more asymmetric in gas velocity fields than their controls. These observational evidences point to the gas accretion scenario followed by angular momentum redistribution from gas-gas collision, leading to gas inflow and central star formation for the SF and GV misaligned galaxies. We propose three possible origins of the misaligned QS galaxies: (1) external gas accretion; (2) merger; (3) GV misaligned galaxies evolve into QS galaxies.
description: 13 pages, 12 figures, accepted for publication in MNRAS
Ionizing Protoplanetary Disks in Pebble Collisions
Creators: name: Wurm, Gerhard
name: Jungmann, Felix
name: Teiser, Jens
Publisher: name: arXiv
Year: 2022
Subjects: subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: FOS: Physical sciences

description: We introduce collisions of solids as a new and efficient ionization mechanism for gas in protoplanetary disks, which especially operates in the dense midplane of protoplanetary disks. This idea is sparked by laboratory experiments where we found that charge, which is exchanged by grains in mutual collision (tribocharging), is not tied to their surfaces alone. As kind of collateral effect, charges also become entrained into the gas phase, i.e. collisions ionize the protoplanetary disk. Therefore, solids are not only sinks of charges in disks but also sources. A first estimate shows that ionization rates in the midplane at 1 AU in the range of $10^{-19} ... 10^{-15} \rm \, s^{-1}$ seem feasible depending on the assumption of rather calm or highly turbulent conditions with radial particle pile up.
description: Accepted for publication by Monthly Notices of the Royal Astronomical Society
AfGT 2021 Annual Report.pdf
Creators: name: TAN, KATINA YEE SHAN
name: KEAMY, RON
name: CLINTON, JANET
Publisher: name: University of Melbourne
Year: 2021
Subjects: Other education not elsewhere classified
Teacher education and professional development of educators

description: Assessment for Graduate Teaching Report 2021: Prepared for the Assessment for Graduate Teaching (AfGT) ConsortiumCollaborators & Licensees
Controlling polarization of spintronic THz emitter by remanent magnetization texture
Creators: name: Wu, Weipeng
name: Lendinez, Sergi
name: Kaffash, Mojtaba Taghipour
name: Schaller, Richard D.
name: Wen, Haidan
name: Jungfleisch, M. Benjamin
Publisher: name: arXiv
Year: 2022
Subjects: subject: Materials Science (cond-mat.mtrl-sci)
subject: Mesoscale and Nanoscale Physics (cond-mat.mes-hall)
subject: Applied Physics (physics.app-ph)
subject: Optics (physics.optics)
subject: FOS: Physical sciences

description: Terahertz (THz) sciences and technologies have contributed to a rapid development of a wide range of applications and expanded the frontiers in fundamental science. Spintronic terahertz emitters offer conceptual advantages since the spin orientation in the magnetic layer can be easily controlled either by the externally applied magnetic field or by the internal magnetic field distribution determined by the specific shape of the magnetic elements. Here, we report a switchable terahertz source based on micropatterned magnetic heterostructures driven by femtosecond laser pulses. We show that the precise tunability of the polarization state is facilitated by the underlying magnetization texture of the magnetic layer that is dictated by the shape of the microstructure. These results also reveal the underlying physical mechanisms of a nonuniform magnetization state on the generation of ultrafast spin currents in the magnetic heterostructures. Our findings indicate that the emission of the linearly polarized THz waves can be switched on and off by saturating the sample using a biasing magnetic field, opening fascinating perspectives for integrated on-chip THz devices with wide-ranging potential applications.
Radio detection of an elusive millisecond pulsar in the Globular Cluster NGC 6397
Creators: name: Zhang, Lei
name: Ridolfi, Alessandro
name: Blumer, Harsha
name: Freire, Paulo
name: Manchester, Richard N.
name: McLaughlin, Maura
name: Kremer, Kyle
name: Cameron, Andrew D.
name: Zhang, Zhiyu
name: Behrend, Jan
name: Burgay, Marta
name: Buchner, Sarah
name: Champion, David J.
name: Chen, Weiwei
name: Dai, Shi
name: Feng, Yi
name: Fu, Xiaoting
name: Guo, Meng
name: Hobbs, George
name: Keane, Evan F.
name: Kramer, Michael
name: Levin, Lina
name: Li, Xiangdong
name: Ni, Mengmeng
name: Pan, Jingshan
name: Padmanabh, Prajwal V.
name: Possenti, Andrea
name: Ransom, Scott M.
name: Tsai, Chao-Wei
name: Krishnan, Vivek Venkatraman
name: Wang, Pei
name: Zhang, Jie
name: Zhi, Qijun
name: Zhang, Yongkun
name: Li, Di
Publisher: name: arXiv
Year: 2022
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: We report the discovery of a new 5.78 ms-period millisecond pulsar (MSP), PSR J1740-5340B (NGC 6397B), in an eclipsing binary system discovered with the Parkes radio telescope (now also known as Murriyang), Australia, and confirmed with the MeerKAT radio telescope in South Africa. The measured orbital period, 1.97 days, is the longest among all eclipsing binaries in globular clusters (GCs) and consistent with that of the coincident X-ray source U18, previously suggested to be a 'hidden MSP'. Our XMM-Newton observations during NGC 6397B's radio quiescent epochs detected no X-ray flares. NGC 6397B is either a transitional MSP or an eclipsing binary in its initial stage of mass transfer after the companion star left the main sequence. The discovery of NGC 6397B potentially reveals a subgroup of extremely faint and heavily obscured binary pulsars, thus providing a plausible explanation to the apparent dearth of binary neutron stars in core-collapsed GCs as well as a critical constraint on the evolution of GCs.
AfGT 2021 Annual Summary Report
Creators: name: KEAMY, RON
name: CLINTON, JANET
name: TAN, KATINA YEE SHAN
Publisher: name: University of Melbourne
Year: 2021
Subjects: Other education not elsewhere classified
Teacher education and professional development of educators

description: Assessment for Graduate Teaching Summary Report 2021: Prepared for the Assessment for Graduate Teaching (AfGT) Consortium Collaborators & Licensees
British Gallup Poll CQ 979
Creators: name: Social Surveys (Gallup Poll) Limited
Publisher: name: Roper Center for Public Opinion Research
Year: 2022

description: Government approval (1); Harold Wilson performance (1); Margaret Thatcher performance (1); Jeremy Thorpe performance (1); party support (1); last general election (2); urgent problems (2); best party to handle problems (1); next general election (2); party with best policies (1); party with best leaders (1); party unity (2); party concerns (4); Labor politicians (12); conservative politicians (14); politician television appearances (3); government's price & income policy (9); imported food (33); Cup-a-Soup (10); conservation organizations (9); book covers (1); shirt purchase (3).
Outflows and spectral evolution in the eclipsing AMXP SWIFT J1749.4-2807 with NICER, XMM-Newton and NuSTAR
Creators: name: Marino, A.
name: Anitra, A.
name: Mazzola, S. M.
name: Di Salvo, T.
name: Sanna, A.
name: Bult, P.
name: Guillot, S.
name: Mancuso, G.
name: Ng, M.
name: Riggio, A.
name: Albayati, A. C.
name: Altamirano, D.
name: Arzoumanian, Z.
name: Burderi, L.
name: Cabras, C.
name: Chakrabarty, D.
name: Deiosso, N.
name: Gendreau, K. C.
name: Iaria, R.
name: Manca, A.
name: Strohmayer, T. E.
Publisher: name: arXiv
Year: 2022
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: The neutron star low-mass X-ray binary SWIFT J1749.4-2807 is the only known eclipsing accreting millisecond X-ray pulsar. In this manuscript we perform a spectral characterization of the system throughout its 2021, two-week-long outburst, analyzing 11 NICER observations and quasi-simultaneous XMM-Newton and NuSTAR single observations at the outburst peak. The broadband spectrum is well-modeled with a black body component with a temperature of $\sim$0.6 keV, most likely consistent with a hot spot on the neutron star surface, and a Comptonisation spectrum with power-law index $Γ\sim 1.9$, arising from a hot corona at $\sim$12 keV. No direct emission from the disc was found, possibly due to it being too cool. A high truncation radius for the disc, i.e., at $\sim$20--30 R$_{G}$ , was obtained from the analysis of the broadened profile of the Fe line in the reflection component. The significant detection of a blue-shifted Fe XXVI absorption line at $\sim$7 keV indicates weakly relativistic X-ray disc winds, which are typically absent in the hard state of X-ray binaries. By comparing the low flux observed during the outburst and the one expected in a conservative mass-transfer, we conclude that mass-transfer in the system is highly non-conservative, as also suggested by the wind detection. Finally, using the Nicer spectra alone, we followed the system while it was fading to quiescence. During the outburst decay, as the spectral shape hardened, the hot spot on the neutron star surface cooled down and shrank, a trend which could be consistent with the pure power-law spectrum observed during quiescence.
description: 15 pages, 9 figure; accepted for publication on MNRAS
Morphology, color-magnitude and scaling relations of galaxies in Abell 426
Creators: name: Khanday, Sheeraz A.
name: Saha, Kanak
name: Iqbal, Nasser
name: Dhiwar, Suraj
name: Pahwa, Isha
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: We present photometric properties of 183 member galaxies in the Abell 426 cluster using the Sloan Digital Sky Survey (SDSS) imaging and spectroscopic observation. Detailed morphology based on visual classification followed by multi-component image decomposition of 179 galaxies is presented in the SDSS g, r, i-bands. More than 80 percent of the members are Early-type galaxies (ETGs), with elliptical, dwarf elliptical (dE), and lenticular morphology and follow the red-sequence in the color-magnitude diagram (CMD). With a few dEs and spirals in the blue cloud, the cluster CMD is nearly unimodal.The dEs are $\sim2$-mag fainter and follow a different Sersic index and central velocity dispersion distribution than their bright counterparts. Further, we establish the Kormendy relation (KR) and the Fundamental Plane relation (FPR) for 5 different samples of ETGs constructed based on derived physical parameters such as Sersic index, concentration, central velocity dispersion in g, r, i-bands. The mean r-band slope and zero-point of the KR are $3.02\pm0.1$ and $18.65\pm0.03$ in close agreement to other cluster ellipticals in the local and higher redshift. Kinematics-based ETG sample produces the least scatter in KR with zero-point getting brighter by $\sim1.3$-mag from g to i band. The dEs and other low-mass ETGs follow the KR with a similar slope but with $\sim1.3$-mag fainter zero-point and form a parallel KR. The bright ellipticals follow an FPR with $a=1.37\pm0.003$, $b=0.35\pm0.05$ and $c=- 9.37\pm0.02$ in the r-band; galaxies tend to deviate from this relation at the low-mass end. A catalog with morphology and 2D structural analysis is available online.
description: 19 pages, 25 figures, 5 tables, Accepted for publication in MNRAS
Milky Way-like galaxies: stellar population properties of dynamically defined disks, bulges and stellar halos
Creators: name: Ortega-Martinez, Sara
name: Obreja, Aura
name: Dominguez-Tenreiro, Rosa
name: Pedrosa, Susana
name: Rosas-Guevara, Yetli
name: Tissera, Patricia
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: The formation of galaxies can be understood in terms of the assembly patterns of each type of galactic component. To perform this kind of analysis, is necessary to define some criteria to separate those components. Decomposition methods based on dynamical properties are more physically motivated than photometry-based ones. We use the unsupervised Gaussian Mixture model of \texttt{galactic structure finder} to extract the components of a sub-sample of galaxies with Milky Way-like masses from the EAGLE simulations. A clustering in the space of first and second order dynamical moments of all identified substructures reveals five types of galaxy components: thin and thick disks, stellar halos, bulges and spheroids. We analyse the dynamical, morphological and stellar population properties of these five component types, exploring to what extent these properties correlate with each other, and how much they depend on the total galaxy stellar and dark matter halo masses. All galaxies contain a bulge, a stellar halo and a disk. 60% of objects host two disks (thin and thick), and 68% host also a spheroid. The dynamical disk-to-total ratio does not depend on stellar mass, but the median rotational velocities of the two disks do. Thin disks are well separated in stellar ages, [Fe/H] and $α$-enhancement from the three dispersion-dominated components, while thick disks are in between. Except for thin disks, all components show correlations among their stellar population properties: older ages mean lower metallicities and larger $α$-enhancement. Finally, we quantify the weak dependence of stellar population properties on each component's dynamics.
description: 20 pages, 18 figures. Accepted for publication in MNRAS
title: Enzyme - Die Baumeister des Lebens
Creators: name: Neurobiologie, Zoologisches
name: Gllareva, Adelina
name: Hadam, Laura
Publisher: name: Universitätsbibliothek Braunschweig
Year: 2025
Subjects: subject: Stream
subject: TIDig
subject: Open Educational Resources (OERs)
subject: 57

description: Teach It Digital OER (TIDig)
Milky Way Mass with K Giants and BHB Stars Using LAMOST, SDSS/SEGUE, and Gaia: 3D Spherical Jeans Equation and Tracer Mass Estimator
Creators: name: Bird, Sarah A.
name: Xue, Xiang-Xiang
name: Liu, Chao
name: Flynn, Chris
name: Shen, Juntai
name: Wang, Jie
name: Yang, Chengqun
name: Zhai, Meng
name: Zhu, Ling
name: Zhao, Gang
name: Tian, Hai-Jun
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: We measure the enclosed Milky Way mass profile to Galactocentric distances of $\sim70$ and $\sim50$ kpc using the smooth, diffuse stellar halo samples of Bird et al. The samples are LAMOST and SDSS/SEGUE K giants (KG) and SDSS/SEGUE blue horizontal branch (BHB) stars with accurate metallicities. The 3D kinematics are available through LAMOST and SDSS/SEGUE distances and radial velocities and {\it Gaia} DR2 proper motions. Two methods are used to estimate the enclosed mass: 3D spherical Jeans equation and Evans et al. tracer mass estimator (TME). We remove substructure via the Xue et al. method based on integrals of motion. We evaluate the uncertainties on our estimates due to random sampling noise, systematic distance errors, the adopted density profile, and non-virialization and non-spherical effects of the halo. The tracer density profile remains a limiting systematic in our mass estimates, although within these limits we find reasonable agreement across the different samples and the methods applied. Out to $\sim70$ and $\sim50$ kpc, the Jeans method yields total enclosed masses of $4.3\pm0.95$ (random) $\pm0.6$ (systematic) $\times10^{11}$ M$_\odot$ and $4.1\pm1.2$ (random) $\pm0.6$ (systematic) $\times10^{11}$ M$_\odot$ for the KG and BHB stars, respectively. For the KG and BHB samples we find a dark matter virial mass of $M_{200}=0.55^{+0.15}_{-0.11}$ (random) $\pm0.083$ (systematic) $\times10^{12}$ M$_\odot$ and $M_{200}=1.00^{+0.67}_{-0.33}$ (random) $\pm0.15$ (systematic) $\times10^{12}$ M$_\odot$, respectively.
description: Accepted for publication in MNRAS. Comments welcomed
Abundance stratification in type Ia supernovae -- VI: the peculiar slow decliner SN\,1999aa
Creators: name: Aouad, Charles J.
name: Mazzali, Paolo A.
name: Hachinger, Stephan
name: Teffs, Jacob
name: Pian, Elena
name: Ashall, Chris
name: Benetti, Stefano
name: Filippenko, Alexei V.
name: Tanaka, Masaomi
Publisher: name: arXiv
Year: 2022
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: The abundance distribution in the ejecta of the peculiar slowly declining Type Ia supernova (SN\,Ia) SN\,1999aa is obtained by modelling a time series of optical spectra. Similar to SN\,1991T, SN\,1999aa was characterised by early-time spectra dominated by \FeIII\ features and a weak \SiII\,6355\,Å line, but it exhibited a high-velocity \CaII\,H\&K line and morphed into a spectroscopically normal SN\,Ia earlier. Three explosion models are investigated, yielding comparable fits. The innermost layers are dominated by $\sim 0.3$\,\Msun\ of neutron-rich stable Fe-group elements, mostly stable iron. Above that central region lies a \Nifs-dominated shell, extending to $v \approx 11,000$ -- $12,000$\,\kms, with mass $\sim 0.65$\,\Msun. These inner layers are therefore similar to those of normal SNe\,Ia. However, the outer layers exhibit composition peculiarities similar to those of SN\,1991T: the intermediate-mass elements shell is very thin, containing only $\sim 0.2$\,\Msun, and is sharply separated from an outer oxygen-dominated shell, which includes $\sim 0.22$\,\Msun. These results imply that burning suddenly stopped in SN\,1999aa. This is a feature SN\,1999aa shares with SN\,1991T, and explain the peculiarities of both SNe, which are quite similar in nature apart from the different luminosities. The spectroscopic path from normal to SN\,1991T-like SNe\,Ia cannot be explained solely by a temperature sequence. It also involves composition layering differences, suggesting variations in the progenitor density structure or in the explosion parameters.
description: 19 pages, 21 figures
Achillea crithmifolia Waldst. & Kit.
Creators: name: Info Flora
Publisher: name: Zenodo
Year: 2021
Subjects: Biodiversity
Taxonomy
Plantae
Tracheophyta
Magnoliopsida
Asterales
Asteraceae
Achillea
Achillea crithmifolia

description: Achillea crithmifolia Waldst. & Kit.
Meerfenchelblättrige Schafgarbe
Art ISFS: 1250 Checklist: 1000220 Asteraceae Achillea Achillea crithmifolia Waldst. & Kit.
Bestimmungsschlüssel
ZusammenfassungKEINE ANGABE
Ökologie
Lebensraum Lebensraumnach Delarze & al. 2015
KEINE ANGABE
Ökologische Zeigerwerte nach Landolt & al. (2010)
BodenfaktorenKlimafaktorenSalztoleranzFeuchtezahl F--Lichtzahl L--Salzzeichen--Reaktionszahl R--Temperaturzahl T--Nährstoffzahl N--Kontinentalitätszahl K--
Nomenklatur
Gültiger Name (Checklist 2017):Achillea crithmifoliaWaldst. & Kit.
Volksname Deutscher Name: Meerfenchelblättrige Schafgarbe Nom français: Achillée à feuilles de criste marine Nome italiano: Millefoglie con foglie simili al finocchio marino
Übereinstimmung mit anderen Referenzwerken
RelationNomReferenzwerkeNo=Achillea crithmifolia Waldst. & Kit.Checklist 20171250
= Taxon stimmt mit akzeptiertem Taxon überein (Checklist 2017)  Taxon enthält (neben anderen) auch das akzeptierte Taxon (Checklist 2017)
Kommentare aus der Checklist 2017 Neues Taxon: Gegenüber SISF-2 neu aufgenommener Neophyt. Checklist
Status Indigenat: Neophyt: nach der Entdeckung von Amerika in der Region aufgetreten (nach 1500)
Liste der gefährdeten Pflanzen IUCN(nach Walter & Gillett 1997): Nein
description: Published as part of Info Flora, 2021,