bluuebunny/crossref_metadata_2025_split huggingface dataset:
Multiple New or Updated Satellite Total Solar Irradiance (TSI) Composites (1978–2023)
Authors: Connolly Ronan , Soon Willie , Connolly Michael , Cionco Rodolfo Gustavo , Elias Ana G. , Henry Gregory W. , Scafetta Nicola , Velasco Herrera Víctor M. 
Published: October 2024

Abstract
Several total solar irradiance (TSI) satellite missions have been carried out since 1978. None of these missions have lasted more than one to two solar cycles (SCs), and each mission implies a slightly different absolute TSI baseline. Nonetheless, several satellite composites have been developed by compositing satellite data from different missions to form an almost continuous daily record for the satellite era. However, disconcertingly, each mission has implied slightly different changes in TSI between consecutive solar minima and solar maxima. Some groups have developed adjustments to individual missions that have substantially reduced these differences. Others prefer to use the original data published by the satellite science teams. Some TSI composites average together conflicting records, while others prioritize specific records over others. Here, we compare four existing composites to 17 new alternative series based on the available satellite data. These 21 TSI series are statistically sorted into six groups of three to four series each. We found that the six groups suggest different intercycle trends between solar minima. We compare the groups to eight daily resolved solar proxy-based TSI reconstructions and to daily sunspot numbers. Excellent agreement is obtained over one to two SCs, but significant differences are observed over longer timescales for each group. Therefore, we have assembled all these time series (old and new) into a large and new TSI data set for use by the scientific community. Versions scaled to 1 au (for studying solar variability) or in situ values at Earth (for studying solar/terrestrial interactions) are provided at daily, monthly, and yearly resolutions.
New Insights into Type-I Solar Noise Storms from High Angular Resolution Spectroscopic Imaging with the Upgraded Giant Metrewave Radio Telescope
Authors: Mondal Surajit , Kansabanik Devojyoti , Oberoi Divya , Dey Soham 
Published: October 2024

Abstract
Type-I solar noise storms are perhaps the most commonly observed active radio emissions from the Sun at meter-wavelengths. Noise storms have a long-lived and wideband continuum background with superposed islands of much brighter narrowband and short-lived emissions, known as type-I bursts. There is a serious paucity of studies focusing on the morphology of these two types of emissions, primarily because of the belief that coronal scattering will always wash out any features at small angular scales. However, it is important to investigate their spatial structures in detail to make a spatio-temporal connection with observations at extreme-ultraviolet/X-ray bands to understand the detailed nature of these emissions. In this work, we use high angular resolution observations from the upgraded Giant Metrewave Radio Telescope to demonstrate that it is possible to detect structures with angular scales as small as ∼9″, about three times smaller than the smallest structure reported to date from noise storms. Our observations also suggest that while the individual type-I bursts are narrowband in nature, the bursts are probably caused by traveling disturbance(s) inducing magnetic reconnections at different coronal heights, and thus leading to correlated change in the morphology of the type-I bursts observed at a wide range of frequencies.
TIC 435850195: The Second Triaxial Tidally Tilted Pulsator
Authors: Jayaraman Rahul , Rappaport Saul A. , Powell Brian , Handler Gerald , Omohundro Mark , Gagliano Robert , Kostov Veselin , Fuller Jim , Kurtz Donald W. , Zhang Valencia , Ricker George 
Published: October 2024

Abstract
The Transiting Exoplanet Survey Satellite (TESS) has enabled the discovery of numerous tidally tilted pulsators (TTPs), which are pulsating stars in close binaries where the presence of a tidal bulge has the effect of tilting the primary star’s pulsation axes into the orbital plane. Recently, the modeling framework developed to analyze TTPs has been applied to the emerging class of triaxial pulsators, which exhibit nonradial pulsations about three perpendicular axes. In this work, we report on the identification of the second-ever discovered triaxial pulsator, with 16 robustly detected pulsation multiplets, of which 14 are dipole doublets separated by 2ν
orb. We jointly fit the spectral energy distribution and TESS light curve of the star, and find that the primary is slightly evolved off the zero-age main sequence, while the less massive secondary still lies on the zero-age main sequence. Of the 14 doublets, we associate eight with Y
10x
modes and six with novel Y
10y
modes. We exclude the existence of Y
11x
modes in this star and show that the observed pulsation modes must be Y
10y
. We also present a toy model for the triaxial pulsation framework in the context of this star. The techniques presented here can be utilized to rapidly analyze and confirm future triaxial pulsator candidates.
The Manhattan Suite: Accelerated Galaxy Evolution in the Early Universe
Authors: Rennehan Douglas 
Published: October 2024

Abstract
Observational advances have allowed the detection of galaxies, protoclusters, and galaxy clusters at higher and higher redshifts, opening a new view into extreme galaxy evolution. I present an argument that the high-redshift, massive galaxies discovered over the last decade are really the most massive galaxies within protocluster cores of galaxy clusters at z ∼ 2, and that they are the partial descendants of same galaxies discovered by JWST at z ∼ 9. To that end, I present The Manhattan Suite, a set of 100 high resolution zoom-in simulations of the most massive galaxy clusters, out to 9 R
vir, selected at z = 2 from a (1.5 cGpc)3 parent volume, and simulated using the simba model. Unlike other cluster suites, my selection at z = 2 ensures that these systems are biased in a similar fashion to observations, in that they should be the brightest and the most massive by construction at z ≳ 2. I show that my sample is able to reproduce extremely star-bursting protoclusters such as SPT2349-56, high-redshift galaxy clusters XLSSC122 and JKCS041, and the wealth of massive (sometimes quenched) galaxies at z ≳ 3 and up to z ∼ 9. I argue that these systems are intimately linked, and represent the same evolutionary history.
Full Stokes-vector Inversion of the Solar Mg ii h and k Lines
Authors: Li Hao , del Pino Alemán Tanausú , Trujillo Bueno Javier 
Published: October 2024

Abstract
The polarization of the Mg ii h and k resonance lines is the result of the joint action of scattering processes and the magnetic field–induced Hanle, Zeeman, and magneto-optical effects, thus holding significant potential for the diagnostic of the magnetic field in the solar chromosphere. The Chromospheric LAyer Spectro-Polarimeter sounding-rocket experiment, carried out in 2019, successfully measured at each position along the 196″ spectrograph slit the wavelength variation of the four Stokes parameters in the spectral region of this doublet around 280 nm, both in an active-region plage and in a quiet region close to the limb. We consider some of these CLASP2 Stokes profiles and apply to them the recently developed HanleRT Tenerife Inversion Code, which assumes a one-dimensional model atmosphere for each spatial pixel under consideration (i.e., it neglects the effects of horizontal radiative transfer). We find that the nonmagnetic causes of symmetry breaking, due to the horizontal inhomogeneities and the gradients of the horizontal components of the macroscopic velocity in the solar atmosphere, have a significant impact on the linear polarization profiles. By introducing such nonmagnetic causes of symmetry breaking as parameters in our inversion code, we can successfully fit the Stokes profiles and provide an estimation of the magnetic field vector. For example, in the quiet region pixels, where no circular polarization signal is detected, we find that the magnetic field strength in the upper chromosphere varies between 1 and 20 G.
Magnetic Fields in a Sample of Planet-hosting M Dwarf Stars from Kepler, K2, and TESS Observed by APOGEE
Authors: Wanderley Fábio , Cunha Katia , Smith Verne V. , Kochukhov Oleg , Souto Diogo , Allende Prieto C. , Mahadevan Suvrath , Majewski Steven R. , Muirhead Philip S. , Pinsonneault Marc , Terrien Ryan 
Published: October 2024

Abstract
Stellar magnetic fields have a major impact on space weather around exoplanets orbiting low-mass stars. From an analysis of Zeeman-broadened Fe i lines measured in near-infrared SDSS/APOGEE spectra, mean magnetic fields are determined for a sample of 29 M dwarf stars that host closely orbiting small exoplanets. The calculations employed the radiative transfer code Synmast and MARCS stellar model atmospheres. The sample M dwarfs are found to have measurable mean magnetic fields ranging between ∼0.2 and ∼1.5 kG, falling in the unsaturated regime on the 〈B〉 versus P
rot plane. The sample systems contain 43 exoplanets, which include 23 from Kepler, nine from K2, and nine from Transiting Exoplanet Survey Satellite. We evaluated their equilibrium temperatures, insolation, and stellar habitable zones and found that only Kepler-186f and TOI-700d are inside the habitable zones of their stars. Using the derived values of 〈B〉 for the stars Kepler-186 and TOI-700 we evaluated the minimum planetary magnetic field that would be necessary to shield the exoplanets Kepler-186f and TOI-700d from their host star’s winds, considering reference magnetospheres with sizes equal to those of the present-day and young Earth, respectively. Assuming a ratio of 5% between large- to small-scale B-fields, and a young-Earth magnetosphere, Kepler-186f and TOI-700d would need minimum planetary magnetic fields of, respectively, 0.05 and 0.24 G. These values are considerably smaller than Earth’s magnetic field of 0.25 G ≲ B ≲ 0.65 G, which suggests that these two exoplanets might have magnetic fields sufficiently strong to protect their atmospheres and surfaces from stellar magnetic fields.
The State of Solar Wind Heavy Ions in Interplanetary Coronal Mass Ejection–Driven Geomagnetic Storms
Authors: Wang Cong , He Fei , Zhang Xiaoxin 
Published: October 2024

Abstract
During geomagnetic storms, which are the primary periods for heavy ions from the solar wind to enter Earth’s magnetospheric space, the charge state of solar wind heavy ions during these storms has significant implications for studying the distribution and effects of heavy ions in the magnetosphere. We analyzed the states and variations of heavy ions during 158 interplanetary coronal mass ejection (ICME)–driven geomagnetic storm events using data from the Advanced Composition Explorer satellite and examined four of these events in detail. We found that the increase in the average charge state of heavy ions such as O, Mg, Si, and Fe is positively correlated with the intensity of the geomagnetic storm. Regarding the abundance ratio of heavy ions such as Ne, Mg, Si, and Fe relative to oxygen ions, the rate and magnitude of increase in abundance ratios during extreme geomagnetic storms (Kp = 9) triggered by ICME events are significantly higher than those during other levels of geomagnetic storms. Additionally, we observed that although the average charge states of heavy ions such as O and Fe are correlated with the geomagnetic storm intensity induced by ICMEs, there are significant individual differences in the charge state variations of heavy ions.
Regulation of Solar Wind Electron Temperature Anisotropy by Collisions and Instabilities
Authors: Yoon Peter H. , Salem Chadi S. , Klein Kristopher G. , Martinović Mihailo M. , López Rodrigo A. , Seough Jungjoon , Sarfraz Muhammad , Lazar Marian , Shaaban Shaaban M. 
Published: October 2024

Abstract
Typical solar wind electrons are modeled as being composed of a dense but less energetic thermal “core” population plus a tenuous but energetic “halo” population with varying degrees of temperature anisotropies for both species. In this paper, we seek a fundamental explanation of how these solar wind core and halo electron temperature anisotropies are regulated by combined effects of collisions and instability excitations. The observed solar wind core/halo electron data in (β
∥, T
⊥/T
∥) phase space show that their respective occurrence distributions are confined within an area enclosed by outer boundaries. Here, T
⊥/T
∥ is the ratio of perpendicular and parallel temperatures and β
∥ is the ratio of parallel thermal energy to background magnetic field energy. While it is known that the boundary on the high-β
∥ side is constrained by the temperature anisotropy-driven plasma instability threshold conditions, the low-β
∥ boundary remains largely unexplained. The present paper provides a baseline explanation for the low-β
∥ boundary based upon the collisional relaxation process. By combining the instability and collisional dynamics it is shown that the observed distribution of the solar wind electrons in the (β
∥, T
⊥/T
∥) phase space is adequately explained, both for the “core” and “halo” components.
A Physically Motivated Framework to Compare the Merger Timescales of Isolated Low- and High-mass Galaxy Pairs Across Cosmic Time
Authors: Chamberlain Katie , Patel Ekta , Besla Gurtina , Torrey Paul , Rodriguez-Gomez Vicente 
Published: October 2024

Abstract
The merger timescales of isolated low-mass pairs (108 < M
* < 5 × 109
M
⊙) on cosmologically motivated orbits have not yet been studied in detail, though isolated high-mass pairs (5 × 109 < M
* < 1011
M
⊙) have been studied extensively. It is common to apply the same separation criteria and expected merger timescales of high-mass pairs to low-mass systems, however, it is unclear if their merger timescales are similar, or if they evolve similarly with redshift. We use the Illustris TNG100 simulation to quantify the merger timescales of isolated low-mass and high-mass major pairs as a function of cosmic time, and explore how different selection criteria impact the mass and redshift dependence of merger timescales. In particular, we present a physically motivated framework for selecting pairs via a scaled separation criterion, wherein pair separations are scaled by the virial radius of the primary’s Friends-of-Friends (FoF) group halo (r
sep < 1 R
vir). Applying these scaled separation criteria yields equivalent merger timescales for both mass scales at all redshifts. Alternatively, static physical separation selections applied equivalently to all galaxy pairs at all redshifts lead to a difference in merger rate of up to ∼1 Gyr between low- and high-mass pairs, particularly for r
sep < 150 kpc. As a result, applying the same merger timescales to physical-separation-selected pairs will lead to a bias that systematically overpredicts low-mass galaxy merger rates.
The Faraday Rotation Measure of the M87 Jet at 3.5 mm with ALMA
Authors: Peng Sijia , Lu Ru-Sen , Goddi Ciriaco , Krichbaum Thomas P. , Li Zhiyuan , Liu Ruo-Yu , Kim Jae-Young , Nakamura Masanori , Yuan Feng , Chen Liang , Martí-Vidal Iván , Shen Zhiqiang 
Published: October 2024

Abstract
Faraday rotation is an important probe of the magnetic fields and magnetized plasma around active galactic nuclei jets. We present a Faraday rotation measure (RM) image of the M87 jet between 85.2 and 101.3 GHz with a resolution of ∼2″ with the Atacama Large Millimeter/submillimeter Array. We found that the RM of the M87 core is (4.5 ± 0.4) × 104 rad m−2 with a low linear polarization fraction of (0.88 ± 0.08)%. The spatial RM gradient in the M87 jet spans a wide range from ∼ −2 × 104 rad m−2 to ∼3 × 104 rad m−2 with a typical uncertainty of 0.3 × 104 rad m−2. A comparison with previous RM measurements of the core suggests that the Faraday rotation of the core may originate very close to the supermassive black hole. Both an internal origin and an external screen with a rapidly varying emitting source could be possible. As for the jet, the RM gradient indicates a helical configuration of the magnetic field that persists up to the kiloparsec scale. Combined with the kiloparsec-scale RM measurements at lower frequencies, we found that RM is frequency-dependent in the jet. One possible scenario to explain this dependence is that the kiloparsec-scale jet has a trumpet-like shape, and the jet coil unwinds near its end.
Witt’s Hyperbola Is Both Predicted and Observed to Pass Close to the Lensing Galaxies in Quadruple Quasars
Authors: Schechter Paul L. , Luhtaru Richard 
Published: October 2024

Abstract
When a rectangular hyperbola is constructed from the image positions of a quadruply lensed quasar, as proposed by Witt, it passes very close to the lensing galaxy. The median measured perpendicular offset between the observed light center of the lens and Witt’s hyperbola is 0.″013 for a sample for 39 systems lensed by a relatively isolated galaxy. The family of lens models adopted by Witt predicts that the lens lies on the hyperbola, but its position is not used for its construction. The median offset corresponds to roughly 1% of the Einstein ring radius and suggests that the centers of the lensing potential are close to the light centers of the lens. By putting a restrictive prior on the perpendicular distance to Witt’s hyperbola (or on the distance between the galaxy and the potential), one reduces by one the dimensionality of a model space when fitting data. Taking the brightest pixel of a lensing galaxy as its center avoids a shortcoming of using the average light center for a constraint.
Papaver recircumscribed: A review of neighbouring Papaveraceae genera, including Afropapaver nom. et stat. nov. and Oreomecon, a large, Arctic-Alpine genus
Authors: Elvebakk Arve , Bjerke Jarle W. 
Published: October 2024

Papaveraceae tribus Papavereae includes an American and a mainly Eurasian group of genera. The latter is proposed here to include eight genera. Amongst these, the recently described genus Oreomecon is phylogenetically a sister group to Meconopsis, a genus from Himalaya and central China, which is reviewed here as including 95 species and 21 subspecies. By contrast, Oreomecon has a circumpolar northern alpine and Arctic distribution, including incompletely understood taxa, many threatened by climatic warming. Based on a review of literature and phylogenies, it is proposed here that Oreomecon includes 68 species and 29 subspecies. Oreomecon aurantiaca, O. cornwallisensis, O. keelei, O. ochotensis and O. uschakovii, 29 subspecies and four varieties are placed in Oreomecon here, 29 of these as recombinations, the remaining ones as nomenclatural novelties. A total of 21 existing Oreomecon names are placed into synonymy. The taxonomically challenging O. alpina group from Central Europe is treated as comprising three species, with the remaining entities positioned at the subspecies level pending further studies. The much-studied Nordic species O. radicata is treated with eight subspecies here, based on morphometric studies, whereas four accepted entities are provisionally recombined at the variety level. The name Papaver tenellum and the basionyms of Oreomecon alborosea, O. alpina subsp. corona-sancti-stephani, O. alpina subsp. degenii, O. anomala, O. lapeyrouseana subsp. endressii, O. lapponica subsp. laestadiana and O. nivalis are lectotypified here. Two replacement names, Oreomecon alpina subsp. markgrafiana and O. radicata subsp. knabeniana, are introduced.
Papaver, as currently understood, is recircumscribed here to represent four genera. The isolated section Horrida, from southern Africa, is raised to genus level with the new name Afropapaver and its only species is recombined as Afropapaver aculeatum. Papaver sect. Californica from California and adjacent Mexico is treated as the genus Stylomecon. The name has been applied to one of the two species of this group and we now recombine the other one as S. crassifolia, based on an older basionym replacing Papaver californicum. Papaver cambricum is accepted in its alternative position as the monotypic genus Parameconopsis. As reviewed here, Papaver comprises 59 species and 14 subspecies and is only the third-largest genus in the group. Based on the distribution of its closest relatives and oldest sections, it is hypothesised here that Papaver arose in the western Mediterranean. Its poricidal capsule dehiscence serves as an excellent adaptation to seed dispersal in open, arid environments, possibly explaining its later success in the Türkiye-Caucasus-Middle East area, where its diversity both at species and section level is highest.
L'évolution de la sécheresse météorologique dans la partie centrale de la plaine de la Beqaa (Liban) : enseignements de l'indice standardisé de précipitations sur la période 1933-2020 dans le secteur Rayak - Tal Amara
Authors: Karam Georges 
Published: October 2024

L'étude porte sur l'évolution temporelle de la sécheresse météorologique dans un territoire agricole semi-aride situé au cœur de la plaine de la Beqaa au Liban. Pour caractériser cet aléa climatique, c'est l'Indice Standardisé de Précipitation (SPI), préconisé par l'Organisation Météorologique Mondiale, qui a été utilisé. Cet indice, appuyé sur les seules données pluviométriques, a été calculé à trois échelles temporelles (12, 6 et 3 mois) sur une période allant de septembre 1933 à août 2020.Les résultats obtenus à partir des données annuelles (SPI-12) et de celles pour les semestres d'octobre à mars (SPI-6) montrent que le secteur d'étude a connu des sécheresses plus fréquentes à partir de 1956-57, avec des successions d'années sèches pouvant couvrir 6, 7 et même 9 années. À l'échelle saisonnière, l'hiver (décembre-février), saison de loin la plus humide, manifeste aussi une diminution des pluies et une multiplication des épisodes secs à partir de 1956-57. En revanche, les données de l'automne et du printemps se distinguent par la présence de deux ruptures, la première (1962-63 pour le printemps et 1963-64 pour l'automne) se traduisant par une accentuation des pluies et la seconde (1984-85 pour le printemps et 1996-97 pour l'automne) par une diminution. La fréquence des sécheresses est particulièrement forte depuis la seconde rupture. En dépit de leur grand nombre, les sécheresses sont restées d'intensité limitée. Même en 2013-14, année la plus sèche de la série, seul le semestre octobre-mars a été extrêmement sec (SPI de -2,03). À toutes les échelles temporelles, les sécheresses légères (SPI < -1,0) ont été très largement majoritaires.
Pontian Hellenism in continuous “exodus” – prosfygia. Testimonies and interviews
Authors: Charitidou Georgia I. 
Published: October 2024

Hellenism, established on the shores of the Black Sea (Greek Pontus) since ancient times (8th century BC colonization), preserved the Greek language and the Greek Spirit. The end of this era in the Pontus region, came after coordinated persecutions, displacements and the Turkification of populations as well as coercive works during the Ottoman Empire; Intensified after the dominance of the Young Turks and Kemal, at the beginning of the 20th century (1913-1923 AD). Over this decade, the Pontus Greeks were forced to leave their homes and follow endless death marches. Many fled to Southern Russia, where under Stalin they faced new persecutions and deportations with the few survivors eventually repatriating to Greece. This continuous “Exodus” – refugee (Greek prosfygia) and its characteristics i.e. losses, problems, adaptation etc, are highlighted by the testimonies of Pontians, which were gathered by the Committee of Pontian Studies, the scientific body of Pontians.