pathfinder: A Semantic Framework for Literature Review and Knowledge Discovery in Astronomy
Paper โข 2408.01556 โข Published โข 3
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|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
12473133 | 1607.01526 | Globular clusters as tracers of the host galaxy mass distribution: the Fornax dSph test case | The Fornax dwarf spheroidal galaxy is the most massive satellites of the Milky Way, claimed to be embedded in a huge dark matter halo, and the only among the Milky Way satellites hosting five globular clusters. Interestingly, their estimated masses, ages and positions seem hardly compatible with the presence of a significant dark matter component, as expected in the ฮCDM scheme. Indeed, if Fornax would have a CDM halo with a standard density profile, all its globular clusters should have sunk to the galactic centre many Gyr ago due to dynamical friction. Due to this, some authors proposed that the most massive clusters may have formed out of Fornax and later tidally captured. In this paper, we investigate the past evolution of the Fornax GC system by using both a recently developed, semi-analytical treatment of dynamical friction and direct N-body simulations of the orbital evolution of the globular clusters within Fornax and of Fornax galaxy around the Milky Way. Our results suggest that an `in situ' origin for all the clusters is likely if their observed positions are close to their spatial ones and their orbits are almost circular. Moreover, the Milky Way seems to accelerate the GC decay reducing the decay time of 15 per cent. Nevertheless, our results indicate that the GCs survival probability exceeds 50 per cent, even in the case of cuspy density profiles. We conclude that more detailed data are required to shed light on the Fornax dark matter content, to distinguish between a cuspy or a cored profile. | [
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-0.... | 9.992026 | 7.407736 | 2016-07-01 | 17 | 2016MNRAS.461.4335A | [
"cuspy density profiles",
"dynamical friction",
"Fornax GC",
"Fornax",
"the Fornax dark matter content",
"five globular clusters",
"the globular clusters",
"direct N-body simulations",
"the Fornax GC system",
"a huge dark matter halo",
"a standard density profile",
"the Milky Way satellites",
... | [
"methods: numerical",
"galaxies: individual: Fornax",
"galaxies: nuclei",
"galaxies: star clusters: general",
"Astrophysics - Astrophysics of Galaxies"
] | 1 | [
"10.1093/mnras/stw1647",
"10.48550/arXiv.1607.01526"
] | [
"Arca-Sedda, M.",
"Capuzzo-Dolcetta, R."
] | [
"Department of Physics, Sapienza, University of Rome, Piazzale Aldo Moro 5, I-00185 Rome, Italy",
"Department of Physics, Sapienza, University of Rome, Piazzale Aldo Moro 5, I-00185 Rome, Italy"
] | [
"2017MNRAS.464.3060A",
"2017MNRAS.471..478A",
"2018A&A...615A..91B",
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"2018MNRAS.479..900A",
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"2019ApJ...877..133D",
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"2020MNRAS.493..320L",
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5209849 | 1607.03009 | Impacts of fragmented accretion streams onto classical T Tauri stars: UV and X-ray emission lines | Context. The accretion process in classical T Tauri stars (CTTSs) can be studied through the analysis of some UV and X-ray emission lines which trace hot gas flows and act as diagnostics of the post-shock downfalling plasma. In the UV-band, where higher spectral resolution is available, these lines are characterized by rather complex profiles whose origin is still not clear. <BR /> Aims: We investigate the origin of UV and X-ray emission at impact regions of density structured (fragmented) accretion streams. We study if and how the stream fragmentation and the resulting structure of the post-shock region determine the observed profiles of UV and X-ray emission lines. <BR /> Methods: We modeled the impact of an accretion stream consisting of a series of dense blobs onto the chromosphere of a CTTS through two-dimensional (2D) magnetohydrodynamic (MHD) simulations. We explored different levels of stream fragmentation and accretion rates. From the model results, we synthesize C IV (1550 ร
) and O VIII (18.97 ร
) line profiles. <BR /> Results: The impacts of accreting blobs onto the stellar chromosphere produce reverse shocks propagating through the blobs and shocked upflows. These upflows, in turn, hit and shock the subsequent downfalling fragments. As a result, several plasma components differing for the downfalling velocity, density, and temperature are present altoghether. The profiles of C IV doublet are characterized by two main components: one narrow and redshifted to speed โ 50 km s<SUP>-1</SUP> and the other broader and consisting of subcomponents with redshift to speed in the range 200-400 km s<SUP>-1</SUP>. The profiles of O VIII lines appear more symmetric than C IV and are redshifted to speed โ 150 km s<SUP>-1</SUP>. <BR /> Conclusions: Our model predicts profiles of C IV line remarkably similar to those observed and explains their origin in a natural way as due to stream fragmentation. <P />Movies are available at <A href="http://www.aanda.org/10.1051/0004-6361/201628858/olm">http://www.aanda.org</A> | [
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-0.0... | 9.33351 | 12.213435 | 2016-07-01 | 15 | 2016A&A...594A..93C | [
"line profiles",
"C IV line",
"stream fragmentation",
"O VIII lines",
"accretion rates",
"UV and X-ray emission lines",
"dense blobs",
"the post-shock downfalling plasma",
"C IV doublet",
"C IV",
"fragmentation",
"speed",
"shocked upflows",
"impact regions",
"several plasma components",
... | [
"accretion",
"accretion disks",
"magnetohydrodynamics (MHD)",
"stars: pre-main sequence",
"shock waves",
"X-rays: stars",
"ultraviolet: stars",
"Astrophysics - Solar and Stellar Astrophysics"
] | 3 | [
"10.1051/0004-6361/201628858",
"10.48550/arXiv.1607.03009"
] | [
"Colombo, S.",
"Orlando, S.",
"Peres, G.",
"Argiroffi, C.",
"Reale, F."
] | [
"INAF-Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134, Palermo, Italy",
"INAF-Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134, Palermo, Italy",
"INAF-Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134, Palermo, Italy; Dipartimento di Fisica & Chimica,... | [
"2017A&A...598L...8P",
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12586989 | 1607.06240 | Hybrid entropy stable HLL-type Riemann solvers for hyperbolic conservation laws | It is known that HLL-type schemes are more dissipative than schemes based on characteristic decompositions. However, HLL-type methods offer greater flexibility to large systems of hyperbolic conservation laws because the eigenstructure of the flux Jacobian is not needed. We demonstrate in the present work that several HLL-type Riemann solvers are provably entropy stable. Further, we provide convex combinations of standard dissipation terms to create hybrid HLL-type methods that have less dissipation while retaining entropy stability. The decrease in dissipation is demonstrated for the ideal MHD equations with a numerical example. | [
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... | 8.773089 | 4.468664 | 2016-07-01 | 7 | 2017JCoPh.330..566S | [
"hyperbolic conservation laws",
"entropy stability",
"characteristic decompositions",
"standard dissipation terms",
"less dissipation",
"large systems",
"Jacobian",
"HLL",
"greater flexibility",
"dissipation",
"several HLL-type Riemann solvers",
"hybrid HLL-type methods",
"HLL-type schemes",... | [
"Entropy stability",
"Ideal magnetohydrodynamics",
"HLL",
"Riemann solver",
"Discrete entropy inequality",
"Mathematics - Numerical Analysis",
"Astrophysics - Instrumentation and Methods for Astrophysics"
] | 1 | [
"10.1016/j.jcp.2016.10.034",
"10.48550/arXiv.1607.06240"
] | [
"Schmidtmann, Birte",
"Winters, Andrew R."
] | [
"MathCCES, RWTH Aachen University, Schinkelstr. 2, 52062 Aachen, Germany",
"Mathematisches Institut, Universitรคt zu Kรถln, Weyertal 86-90, 50931 Kรถln, Germany"
] | [
"2019JCoPh.378..477S",
"2019ShWav..29..755P",
"2020JCoPh.41609545T",
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168897 | 1607.07246 | Dynamics of Saturnโs great storm of 2010-2011 from Cassini ISS and RPWS | Saturnโs quasi-periodic planet-encircling storms are the largest convecting cumulus outbursts in the Solar System. The last eruption was in 1990 (Sรกnchez-Lavega, A. [1994]. Chaos 4, 341-353). A new eruption started in December 2010 and presented the first-ever opportunity to observe such episodic storms from a spacecraft in orbit around Saturn (Fischer, G. et al. [2011]. Nature 475, 75-77; Sรกnchez-Lavega, A. et al. [2011]. Nature 475, 71-74; Fletcher, L.N. et al. [2011]. Science 332, 1413). Here, we analyze images acquired with the Cassini Imaging Science Subsystem (ISS), which captured the stormโs birth, evolution, and demise. In studying the end of the convective activity, we also analyze the Saturn Electrostatic Discharge (SED) signals detected by the Radio and Plasma Wave Science (RPWS) instrument. The stormโs initial position coincided with that of a previously known feature called the String of Pearls (SoPs) at 33ยฐN planetocentric latitude. Intense cumulus convection at the westernmost point of the storm formed a particularly bright โheadโ that drifted at -26.9 ยฑ 0.8 m s<SUP>-1</SUP> (negative denotes westward motion). On January 11, 2011, the size of the head was 9200 km and up to 34,000 km in the north-south and east-west dimensions, respectively. RPWS measurements show that the longitudinal extent of the lightning source expanded with the stormโs growth. The storm spawned the largest tropospheric vortex ever seen on Saturn. On January 11, 2011, the anticyclone was sized 11,000 km by 12,000 km in the north-south and east-west directions, respectively. Between January and September 2011, the vortex drifted at an average speed of -8.4 m s<SUP>-1</SUP>. We detect anticyclonic circulation in the new vortex. The vortexโs size gradually decreased after its formation, and its central latitude shifted to the north. The stormโs head moved westward and encountered the new anticyclone from the east in June 2011. After the head-vortex collision, the RPWS instrument detected that the SED activities became intermittent and declined over โผ40 days until the signals became undetectable in early August. In late August, the SED radio signals resurged for 9 days. The storm left a vast dark area between 32ยฐN and 38ยฐN latitudes, surrounded by a highly disturbed region that resembles the mid-latitudes of Jupiter. Using ISS images, we also made cloud-tracking wind measurements that reveal differences in the cloud-level zonal wind profiles before and after the storm. | [
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-0.... | 8.500903 | 15.534467 | 2016-07-01 | 74 | 2013Icar..223..460S | [
"such episodic storms",
"early August",
"G. et al",
"โผ40 days",
"L.N. et al",
"A. et al",
"late August",
"Plasma Wave Science",
"SED",
"Jupiter",
"Saturn",
"the SED radio signals",
"motion",
"demise",
"latitudes",
"Saturnโs quasi-periodic planet-encircling storms",
"RPWS",
"-",
"... | [
"Astrophysics - Earth and Planetary Astrophysics"
] | 18 | [
"10.1016/j.icarus.2012.12.013",
"10.48550/arXiv.1607.07246"
] | [
"Sayanagi, Kunio M.",
"Dyudina, Ulyana A.",
"Ewald, Shawn P.",
"Fischer, Georg",
"Ingersoll, Andrew P.",
"Kurth, William S.",
"Muro, Gabriel D.",
"Porco, Carolyn C.",
"West, Robert A."
] | [
"Department of Atmospheric and Planetary Sciences, Hampton University, Hampton, VA 23668, USA; Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA",
"Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA",
... | [
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12408831 | 1607.07888 | Observed Variability at 1 and 4 ฮผm in the Y0 Brown Dwarf WISEP J173835.52+273258.9 | We have monitored photometrically the Y0 brown dwarf WISEP J173835.52+273258.9 (W1738) at both near- and mid-infrared wavelengths. This โฒ1 Gyr old 400 K dwarf is at a distance of 8 pc and has a mass around 5 M <SUB>Jupiter</SUB>. We observed W1738 using two near-infrared filters at ฮป โ 1 ฮผm, Y and J, on Gemini Observatory and two mid-infrared filters at ฮป โ 4 ฮผm, [3.6] and [4.5], on the Spitzer observatory. Twenty-four hours were spent on the source by Spitzer on each of 2013 June 30 and October 30 UT. Between these observations, around 5 hr were spent on the source by Gemini on each of 2013 July 17 and August 23 UT. The mid-infrared light curves show significant evolution between the two observations separated by 4 months. We find that a double sinusoid can be fit to the [4.5] data, where one sinusoid has a period of 6.0 ยฑ 0.1 hr and the other a period of 3.0 ยฑ 0.1 hr. The near-infrared observations suggest variability with a โผ3.0 hr period, although only at a โฒ2ฯ confidence level. We interpret our results as showing that the Y dwarf has a 6.0 ยฑ 0.1 hr rotation period, with one or more large-scale surface features being the source of variability. The peak-to-peak amplitude of the light curve at [4.5] is 3%. The amplitude of the near-infrared variability, if real, may be as high as 5%-30%. Intriguingly, this size of variability and the wavelength dependence can be reproduced by atmospheric models that include patchy KCl and Na<SUB>2</SUB>S clouds and associated small changes in surface temperature. The small number of large features, as well as the timescale for evolution of the features, is very similar to what is seen in the atmospheres of the solar system gas giants. | [
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... | 7.153717 | 12.541796 | 2016-07-01 | 31 | 2016ApJ...830..141L | [
"large features",
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"surface temperature",
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"significant evolution",
"patchy KCl",
"atmospheric models",
"Jupiter</SUB",
"variability",
"evolution",
"The mid-infrared light curves",
"the solar system gas giants",
"a โผ3.0 hr period",
"Gemini... | [
"brown dwarfs",
"stars: atmospheres",
"stars: individual: WISEP J173835.52+273258.9",
"Astrophysics - Solar and Stellar Astrophysics"
] | 10 | [
"10.3847/0004-637X/830/2/141",
"10.48550/arXiv.1607.07888"
] | [
"Leggett, S. K.",
"Cushing, Michael C.",
"Hardegree-Ullman, Kevin K.",
"Trucks, Jesica L.",
"Marley, M. S.",
"Morley, Caroline V.",
"Saumon, D.",
"Carey, S. J.",
"Fortney, J. J.",
"Gelino, C. R.",
"Gizis, J. E.",
"Kirkpatrick, J. D.",
"Mace, G. N."
] | [
"Gemini Observatory, Northern Operations Center, 670 N. A'ohoku Place, Hilo, HI 96720, USA",
"The University of Toledo, 2801 West Bancroft Street, Mailstop 111, Toledo, OH 43606, USA",
"The University of Toledo, 2801 West Bancroft Street, Mailstop 111, Toledo, OH 43606, USA",
"The University of Toledo, 2801 W... | [
"2016ApJ...832...58E",
"2017ApJ...842...78V",
"2017ApJ...842..118L",
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12518466 | 1607.08820 | "Dispersion by pulsars, magnetars, fast radio bursts and massive electromagnetism at very low radio (...TRUNCATED) | "Our understanding of the universe relies mostly on electromagnetism. As photons are the messengers,(...TRUNCATED) | [-0.00632535619661212,0.011160125955939293,0.012271640822291374,0.01770714297890663,0.00273381313309(...TRUNCATED) | 6.522832 | 3.614386 | 2016-07-01 | 28 | 2017AdSpR..59..736B | ["unknown origin","pulsar observations","Radio astronomy","OLFAR","observations","low frequencies","(...TRUNCATED) | ["Photons","Radio astronomy","Satellites","Pulsars","Magnetars","Fast radio bursts","Astrophysics - (...TRUNCATED) | 6 | [
"10.1016/j.asr.2016.10.018",
"10.48550/arXiv.1607.08820"
] | [
"Bentum, Mark J.",
"Bonetti, Luca",
"Spallicci, Alessandro D. A. M."
] | ["Universiteit van Twente, Faculteit van Elektrotechniek, Wiskunde en Informatica, Telecommunication(...TRUNCATED) | ["2017ApJ...842...23Y","2017CQGra..34u5006S","2017FoPh...47..769A","2017PhLB..764..203B","2017PhLB..(...TRUNCATED) | ["1933PhRv...44..855H","1934PhRv...46.1087B","1934RSPSA.144..425B","1936AnP...418..398E","1936ZPhy..(...TRUNCATED) |
12406228 | 1607.06710 | "Setting the volatile composition of (exo)planet-building material. Does chemical evolution in disk (...TRUNCATED) | "Context. The atmospheres of extrasolar planets are thought to be built largely through accretion of(...TRUNCATED) | [0.008736980147659779,0.01737302727997303,0.059953976422548294,0.0015250288415700197,-0.003882751800(...TRUNCATED) | 10.068603 | 13.044076 | 2016-07-01 | 146 | 2016A&A...595A..83E | ["SUB>2</SUB","interstellar ice abundances","grain surfaces","CO","initial abundances","ices","atomi(...TRUNCATED) | ["astrochemistry","planets and satellites: formation","protoplanetary disks","planets and satellites(...TRUNCATED) | 12 | [
"10.1051/0004-6361/201628509",
"10.48550/arXiv.1607.06710"
] | [
"Eistrup, Christian",
"Walsh, Catherine",
"van Dishoeck, Ewine F."
] | ["Leiden Observatory, Leiden University, PO Box 9513, 2300 RA, Leiden, The Netherlands","Leiden Obse(...TRUNCATED) | ["2017A&A...599A.101V","2017A&A...599A.113M","2017A&A...601A..36B","2017A&A...603A.123H","2017A&A...(...TRUNCATED) | ["1972GeCoA..36..597G","1977Ap&SS..51..153W","1982A&A...114..245T","1983ApJ...267..603P","1993MNRAS.(...TRUNCATED) |
2774767 | 1607.08619 | The Data Reduction Pipeline for the SDSS-IV MaNGA IFU Galaxy Survey | "Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) is an optical fiber-bundle integral-fie(...TRUNCATED) | [-0.018747791647911072,0.03372214362025261,0.015452002175152302,-0.010926260612905025,-0.02956658229(...TRUNCATED) | 11.558285 | 6.853098 | 2016-07-01 | 359 | 2016AJ....152...83L | ["Sloan Digital Sky Survey","MaNGA","individual dithered observations","SDSS-IV Data Release","centr(...TRUNCATED) | ["methods: data analysis","surveys","techniques: imaging spectroscopy","Astrophysics - Instrumentati(...TRUNCATED) | 32 | [
"10.3847/0004-6256/152/4/83",
"10.48550/arXiv.1607.08619"
] | ["Law, David R.","Cherinka, Brian","Yan, Renbin","Andrews, Brett H.","Bershady, Matthew A.","Bizyaev(...TRUNCATED) | ["Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA","Center for As(...TRUNCATED) | ["2016AJ....152..197Y","2016MNRAS.463.2513B","2017AJ....154...28B","2017ApJ...837...32L","2017ApJ...(...TRUNCATED) | ["1969PASP...81..527W","1982PASP...94..715F","1986PASP...98..609H","1996PASP..108..277O","1998ApJ...(...TRUNCATED) |
12585901 | 1607.08157 | Dark matter directional detection: comparison of the track direction determination | "Several directional techniques have been proposed for a directional detection of Dark matter, among(...TRUNCATED) | [0.011932607740163803,0.024745754897594452,0.01089667808264494,0.027581609785556793,-0.0341079644858(...TRUNCATED) | 7.520985 | -2.487568 | 2016-07-01 | 10 | 2017JCAP...01..027C | ["initial direction","different detector materials","crystal detectors","nuclear emulsion plates","W(...TRUNCATED) | ["Astrophysics - Instrumentation and Methods for Astrophysics","Physics - Instrumentation and Detect(...TRUNCATED) | 3 | [
"10.1088/1475-7516/2017/01/027",
"10.48550/arXiv.1607.08157"
] | [
"Couturier, C.",
"Zopounidis, J. P.",
"Sauzet, N.",
"Naraghi, F.",
"Santos, D."
] | ["LPSC, CNRS/IN2P3, UJF, INP, Avenue des Martyrs, 38000, Grenoble, France","LPSC, CNRS/IN2P3, UJF, I(...TRUNCATED) | ["2016arXiv160708765C","2017JInst..12P0009B","2017PhRvD..96h3011O","2020PhRvD.102g5036B","2020PhRvD.(...TRUNCATED) | ["1985PhRvD..31.3059G","1988PhRvD..37.1353S","2003PhLB..571..132S","2010NIMPB.268.1818Z","2012EAS...(...TRUNCATED) |
12509827 | 1607.01847 | Oscillating chiral tensor spectrum from axionic inflation | "We study axionic inflation with a modulated potential and examine if the primordial tensor power sp(...TRUNCATED) | [0.018994921818375587,0.023814870044589043,-0.02079528011381626,-0.005090570542961359,-0.01004440523(...TRUNCATED) | 10.62901 | -1.476708 | 2016-07-01 | 42 | 2016PhRvD..94d4062O | ["chiral gravitational waves","axion phenomenologies","BBO","single-field axion monodromy inflation"(...TRUNCATED) | ["Astrophysics - Cosmology and Nongalactic Astrophysics","General Relativity and Quantum Cosmology",(...TRUNCATED) | 6 | [
"10.1103/PhysRevD.94.044062",
"10.48550/arXiv.1607.01847"
] | [
"Obata, Ippei",
"Soda, Jiro"
] | ["Department of Physics, Kyoto University, Kyoto 606-8502, Japan","Department of Physics, Kobe Unive(...TRUNCATED) | ["2016JCAP...12..031G","2016JHEP...12..137A","2017JCAP...06..050O","2017JCAP...08..005G","2017JHEP..(...TRUNCATED) | ["1990PhRvL..65.3233F","1998PhRvD..57.7089C","2000PhR...331..283M","2001PhRvL..87v1103S","2005IJMPD.(...TRUNCATED) |
End of preview. Expand in Data Studio
This dataset is associated with the Pathfinder app (https://pfdr.app, paper at https://arxiv.org/abs/2408.01556) and is updated roughly monthly to keep pace with new literature in astrophysics and cosmology.
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