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Journal articles on the topic 'North Polar Spur (NPS)'

Author: Grafiati

Published: 6 September 2023

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1

Das, Kaustav K., Catherine Zucker, Joshua S. Speagle, Alyssa Goodman, Gregory M. Green, and João Alves. "Constraining the distance to the North Polar Spur with Gaia DR2." Monthly Notices of the Royal Astronomical Society 498, no. 4 (2020): 5863–72. http://dx.doi.org/10.1093/mnras/staa2702.

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ABSTRACT The North Polar Spur (NPS) is one of the largest structures observed in the Milky Way in both the radio and soft X-rays. While several predictions have been made regarding the origin of the NPS, modelling the structure is difficult without precise distance constraints. In this paper, we determine accurate distances to the southern terminus of the NPS and towards latitudes ranging up to 55°. First, we fit for the distance and extinction to stars towards the NPS using optical and near-infrared photometry and Gaia Data Release 2 astrometry. We model these per-star distance–extinction est

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2

Sofue, Yoshiaki, and Jun Kataoka. "Interaction of the galactic-centre super bubbles with the gaseous disc." Monthly Notices of the Royal Astronomical Society 506, no. 2 (2021): 2170–80. http://dx.doi.org/10.1093/mnras/stab1857.

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ABSTRACT The interaction of Galactic centre (GC) super bubbles (GSBs) with the gaseous disc and halo of the Milky Way is investigated using radio continuum, X-ray, H i, and CO line surveys. The radio North Polar Spur (NPS) constitutes the brightest eastern ridge of GSB, brightening towards the galactic plane and reaching l = 22○, b = +2○ at the sharpest end, where it intersects the tangential direction of the 3-kpc-expanding ring and crater. Examination of the spur ridges reveals that the entire GSB, including the NPS and its counter spurs, constitutes a GC-symmetrical Ω/ Ʊ shape. The thicknes

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3

Yamamoto, Marino, Jun Kataoka, and Yoshiaki Sofue. "Discovery of non-equilibrium ionization plasma associated with the North Polar Spur and Loop I." Monthly Notices of the Royal Astronomical Society 512, no. 2 (2022): 2034–43. http://dx.doi.org/10.1093/mnras/stac577.

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ABSTRACT We investigated the detailed plasma condition of the North Polar Spur (NPS)/Loop I using archival Suzaku data. In previous research, collisional ionization equilibrium (CIE) have been assumed for X-ray plasma state, but we also assume non-equilibrium ionization (NEI) to check the plasma condition in more detail. We found that most of the plasma in the NPS/Loop I favors the state of NEI, and has the density-weighted ionization timescale of net ∼ 1011–12 s cm−3 and the electron number density ne ∼ a few × 10−3 cm−3. The plasma shock age, t, or the time elapsed after the shock front pass

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4

West, J. L., T. L. Landecker, B. M. Gaensler, T. Jaffe, and A. S. Hill. "A Unified Model for the Fan Region and the North Polar Spur: A Bundle of Filaments in the Local Galaxy." Astrophysical Journal 923, no. 1 (2021): 58. http://dx.doi.org/10.3847/1538-4357/ac2ba2.

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Abstract We present a simple, unified model that can explain two of the brightest, large-scale, diffuse, polarized radio features in the sky, the North Polar Spur (NPS) and the Fan Region, along with several other prominent loops. We suggest that they are long, magnetized, and parallel filamentary structures that surround the Local arm and/or Local Bubble, in which the Sun is embedded. We show that this model is consistent with the large number of observational studies on these regions and is able to resolve an apparent contradiction in the literature that suggests that the high-latitude porti

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5

Kataoka, Jun, Yoshiaki Sofue, Yoshiyuki Inoue, Masahiro Akita, Shinya Nakashima, and Tomonori Totani. "X-Ray and Gamma-Ray Observations of the Fermi Bubbles and NPS/Loop I Structures." Galaxies 6, no. 1 (2018): 27. http://dx.doi.org/10.3390/galaxies6010027.

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The Fermi bubbles were possibly created by large injections of energy into the Galactic Center (GC), either by an active galactic nucleus (AGN) or by nuclear starburst more than ~10 Myr ago. However, the origin of the diffuse gamma-ray emission associated with Loop I, a radio continuum loop spanning across 100° on the sky, is still being debated. The northern-most part of Loop I, known as the North Polar Spur (NPS), is the brightest arm and is even clearly visible in the ROSAT X-ray sky map. In this paper, we present a comprehensive review on the X-ray observations of the Fermi bubbles and the

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6

Sofue, Yoshiaki. "The North Polar Spur and Aquila Rift." Monthly Notices of the Royal Astronomical Society 447, no. 4 (2015): 3824–31. http://dx.doi.org/10.1093/mnras/stu2661.

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7

Miroshnichenko, A. P. "THE NORTH POLAR SPUR AS OUR GALAXY JET." Radio Physics and Radio Astronomy 1, no. 2 (2010): 93–98. http://dx.doi.org/10.1615/radiophysicsradioastronomy.v1.i2.10.

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8

LaRocca, Daniel M., Philip Kaaret, K. D. Kuntz, et al. "An Analysis of the North Polar Spur Using HaloSat." Astrophysical Journal 904, no. 1 (2020): 54. http://dx.doi.org/10.3847/1538-4357/abbdfd.

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9

Willingale, R., A. D. P. Hands, R. S. Warwick, S. L. Snowden, and D. N. Burrows. "The X-ray spectrum of the North Polar Spur." Monthly Notices of the Royal Astronomical Society 343, no. 3 (2003): 995–1001. http://dx.doi.org/10.1046/j.1365-8711.2003.06741.x.

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10

Miller, Eric D., Hiroshi Tsunemi, Mark W. Bautz, et al. "Suzaku Observations of the North Polar Spur: Evidence for Nitrogen Enhancement." Publications of the Astronomical Society of Japan 60, sp1 (2008): S95—S106. http://dx.doi.org/10.1093/pasj/60.sp1.s95.

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11

Park, J. W., K. W. Min, K. I. Seon, et al. "Far-Ultraviolet Observations of the Loop I/North Polar Spur Region." Astrophysical Journal 665, no. 1 (2007): L39—L42. http://dx.doi.org/10.1086/521046.

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12

Wolleben, M. "A New Model for the Loop I (North Polar Spur) Region." Astrophysical Journal 664, no. 1 (2007): 349–56. http://dx.doi.org/10.1086/518711.

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13

Milogradov-Tuin, Jelena. "Loop I (the north Polar Spur) region - a quasi radio halo." Symposium - International Astronomical Union 106 (1985): 245–46. http://dx.doi.org/10.1017/s007418090024254x.

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The distribution of total spectral indices between 38 and 408 MHz with a resolution of for δ>-25° has the following main properties:1. Relatively small variations of spectral indices over the sky.2. High indices in the central region at high galactic latitudes.3. Moderately low spectral indices in the anticentre region.4. Lower indices in the low-brightness regions (cold holes).5. The lowest indices in regions containing large amounts of HII.

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14

Gu, Liyi, Junjie Mao, Elisa Costantini, and Jelle Kaastra. "SuzakuandXMM-Newtonobservations of the North Polar Spur: Charge exchange or ISM absorption?" Astronomy & Astrophysics 594 (October 2016): A78. http://dx.doi.org/10.1051/0004-6361/201628609.

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15

Lallement, R., S. Snowden, K. D. Kuntz, et al. "On the distance to the North Polar Spur and the local CO-H2factor." Astronomy & Astrophysics 595 (November 2016): A131. http://dx.doi.org/10.1051/0004-6361/201629453.

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16

Verschuur, G. L., and T. A. Th Spoelstra. "The Need for High Resolution for Polarization Studies of Galactic Background Radiation." Symposium - International Astronomical Union 140 (1990): 62. http://dx.doi.org/10.1017/s0074180900189557.

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Polarization data at 390 and 826 MHz were obtained with the 300-foot telescope in February 1987. A survey of selected regions of sky planned for December 1988 had to be postponed. However, our limited data at 390 MHz show that the 30′ beam detected polarization temperatures between four to six times larger than found in surveys with a 1.3 arcmin resolution. This was true in both the highly polarized region around 1=140 degrees and in the North Polar Spur where polarization structures appear to be unresolved (<0.9 pc at the distance of the spur). High resolution observations will be critical

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17

Sun, X. H., T. L. Landecker, B. M. Gaensler, et al. "FARADAY TOMOGRAPHY OF THE NORTH POLAR SPUR: CONSTRAINTS ON THE DISTANCE TO THE SPUR AND ON THE MAGNETIC FIELD OF THE GALAXY." Astrophysical Journal 811, no. 1 (2015): 40. http://dx.doi.org/10.1088/0004-637x/811/1/40.

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18

Sarkar, Kartick C. "Possible connection between the asymmetry of the North Polar Spur and Loop I and Fermi bubbles." Monthly Notices of the Royal Astronomical Society 482, no. 4 (2018): 4813–23. http://dx.doi.org/10.1093/mnras/sty2944.

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19

Rand, R. J., and S. R. Kulkarni. "Structure of the Local Galactic Magnetic Field." Symposium - International Astronomical Union 140 (1990): 44–46. http://dx.doi.org/10.1017/s007418090018948x.

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We have modeled the local Galactic magnetic field using pulsar rotation measures (RMs), of which there are now about 200 available. The North Polar Spur has a significant effect on pulsar RMs. Using RMs of 116 pulsars nearer than 3 kpc, we find that the local field has a strength B0 = 1.6 ± 0.2 μG toward longitude lB =96° ± 4°, with a reversal of the field at a distance Dr = 600 ± 80 pc toward the inner Galaxy. Relaxing the 3 kpc distance restriction, we find that a concentric ring model with reversals is superior to a bisymmetric spiral model as a fit to the data.

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20

Lallement, Rosine. "North Polar Spur/Loop I: gigantic outskirt of the Northern Fermi bubble or nearby hot gas cavity blown by supernovae?" Comptes Rendus. Physique 23, S2 (2022): 1–24. http://dx.doi.org/10.5802/crphys.97.

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21

Rothenflug, R. "Features in the Soft X-ray Background." International Astronomical Union Colloquium 115 (1990): 146–55. http://dx.doi.org/10.1017/s0252921100012252.

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AbstractThe soft X-ray background is explained in terms of emission coming from hot gas. Most of these soft X-ray data were obtained by proportional counters with a poor energy resolution. Instruments having the capability to resolve lines were only flown by two groups: a GSPC by a Japanese group and a SSD by a french-american collaboration. They both detected the 0 VII line emission coming from the soft X-ray background and so proved the thermal nature of the emission. The implications of these results on possible models for the local hot medium will be discussed. The same detectors observed

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22

Neiman, V. G. "To the projects and challenges of domestic hydrophysical study of the global ocean’s polar regions." Journal of Oceanological Research 48, no. 1 (2020): 5–26. http://dx.doi.org/10.29006/1564-2291.jor-2020.48(1).1.

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One of the climatically significant, but the poor studied hydrophysical factor in the polar regions of the world ocean is the subsurface layer of relatively warm seawater of subtropical origin. In the Arctic Ocean, this layer is associated with the waters of the Gulfstream, the highlatitude continuation of which in the form of a spur of the North Atlantic current penetrates into the Arctic basin, where it sinks to the depth of its density and spreads throughout its vast space in the layer of 100–900 m. The existence of a subsurface layer with an anomalous inversion vertical profile of water te

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23

Panopoulou, G. V., C. Dickinson, A. C. S. Readhead, T. J. Pearson, and M. W. Peel. "Revisiting the Distance to Radio Loops I and IV Using Gaia and Radio/Optical Polarization Data." Astrophysical Journal 922, no. 2 (2021): 210. http://dx.doi.org/10.3847/1538-4357/ac273f.

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Abstract Galactic synchrotron emission exhibits large angular scale features known as radio spurs and loops. Determining the physical size of these structures is important for understanding the local interstellar structure and for modeling the Galactic magnetic field. However, the distance to these structures is either under debate or entirely unknown. We revisit a classical method of finding the location of radio spurs by comparing optical polarization angles with those of synchrotron emission as a function of distance. We consider three tracers of the magnetic field: stellar polarization, po

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24

Soto, Christian, Trisha Ashley, Andrew J. Fox, and Rongmon Bordoloi. "The Signature of the Northern Galactic Center Region in Low-velocity UV Absorption." Astrophysical Journal 954, no. 1 (2023): 64. http://dx.doi.org/10.3847/1538-4357/ace597.

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Abstract The Galactic Center (GC) is surrounded by plasma lobes that extend up to ∼14 kpc above and below the plane. Until now, UV absorption studies of these lobes have only focused on high-velocity components (∣v LSR∣ > 100 km s−1) because low- and intermediate-velocity (LIV) components (∣v LSR∣ < 100 km s−1) are blended with foreground interstellar medium. To overcome this difficulty, we present a differential experiment to compare the LIV absorption between different structures within the GC region, including the Fermi Bubbles (FBs; seen in gamma rays), the eROSITA Bubbles (eBs; seen

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25

Sonett, C. P. "A Supernova Shock Ensemble Model Using Vostok 10Be Radioactivity." Radiocarbon 34, no. 2 (1992): 239–45. http://dx.doi.org/10.1017/s0033822200013680.

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Analysis of the Vostok ice-core record of 10Be (Raisbeck et al. 1987) suggests that the sharply resolved increases in 10Be at 35 ka (kyr) and 60 ka are due to cosmic-ray (CR) increases. As an alternate to long-term solar modulation or strong decreases in the Earth's magnetic field, supernova (SN) forcing is qualitatively consistent with the generation of a forward-reverse shock ensemble from a spherical blast wave of age very approximately at 75 ka. This age agrees with Davelaar, Bleeker and Deerenberg's (1980) identification of 75 ka for the age of a North Polar Spur SN remnant. Confirmation

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26

Lallement, R., L. Capitanio, L. Ruiz-Dern, et al. "Three-dimensional maps of interstellar dust in the Local Arm: using Gaia, 2MASS, and APOGEE-DR14." Astronomy & Astrophysics 616 (August 2018): A132. http://dx.doi.org/10.1051/0004-6361/201832832.

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Context. Gaia data and stellar surveys open the way to the construction of detailed 3D maps of the Galactic interstellar (IS) dust based on the synthesis of star distances and extinctions. Dust maps are tools of broad use, also for Gaia-related Milky Way studies. Aims. Reliable extinction measurements require very accurate photometric calibrations. We show the first step of an iterative process linking 3D dust maps and photometric calibrations, and improving them simultaneously. Methods. Our previous 3D map of nearby IS dust was used to select low-reddening SDSS/APOGEE-DR14 red giants, and thi

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27

Fabian, Stanislaus G., Stephen J. Gallagher, and David De Vleeschouwer. "British–Irish Ice Sheet and polar front history of the Goban Spur, offshore southwest Ireland over the last 250 000 years." Boreas, August 10, 2023. http://dx.doi.org/10.1111/bor.12631.

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Deep Sea Drilling Program (DSDP) Site 548 was cored in 1984 at a water depth of 1256 m on the Goban Spur, offshore southwest Ireland. Coring retrieved a ~100‐m‐thick Pleistocene contourite sequence. This study uses planktonic foraminiferal assemblage and benthic foraminiferal oxygen isotope analyses to establish an age model for the upper 40 m of this core. This site's multidisciplinary analyses of planktonic foraminiferal assemblages, lithic grains, facies and calcium carbonate concentration reveal a 250 000‐year record of the North Atlantic polar front variability and British–Irish Ice Sheet

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28

Mou, G., J. Wu, and Y. Sofue. "Cosmic ray electrons accounting for the North polar spur and the acceleration efficiency of weak shocks." Astronomy & Astrophysics, July 20, 2023. http://dx.doi.org/10.1051/0004-6361/202245401.

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29

Sofue, Yoshiaki. "Giant H i hole inside the 3 kpc ring and the North Polar Spur—The Galactic crater." Publications of the Astronomical Society of Japan 69, no. 5 (2017). http://dx.doi.org/10.1093/pasj/psx067.

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30

Funck, Thomas, and John Shimeld. "Crustal structure and magmatism of the Marvin Spur and northern Alpha Ridge, Arctic Ocean." Geophysical Journal International, December 12, 2022. http://dx.doi.org/10.1093/gji/ggac480.

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Summary The Marvin Spur is a 450-km-long east–west trending escarpment along the northernmost periphery of the Alpha Ridge, starting about 500 km from the coasts of Ellesmere Island and Greenland off the Arctic Ocean margin of North America and running subparallel to the Amerasian margin of the continental Lomonosov Ridge. This region was investigated as part of the Canada-Sweden Polar Expedition in 2016, from which two seismic profiles are presented. The first is a 165-km-long line along the crest of the Marvin Spur. The second is a 221-km-long line extending southwestward from the spur to th

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31

"B. Radio Studies." Transactions of the International Astronomical Union 19, no. 1 (1985): 409–16. http://dx.doi.org/10.1017/s0251107x00006465.

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Several regional surveys of southern HI made with the Argentine 100-m telescope were published (30.155.031). HI and other data were used by Dolidze (30.155. 044) to study the local distribution of gas and star forming regions. The Perseus arm region was the subject of an analogous study by Gerasimenko (34.155.139). Vallée (34.155.005) used rotation measure data from extragalactic sources in the direction of the Perseus arm to determine the magnetic field structure there and to constrain gravitational collapse theories of magnetic compression. HI in the direction of the Puppis window was survey

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32

Thai, Tran Thanh, Nguyen Le Que Lam, Nguyen Thi My Yen, and Ngo Xuan Quang. "Correlation between Oxygen Demand of Nematode Communities with Dissolved Oxygen in the Organic Shrimp Farming Ponds, Ca Mau Province." VNU Journal of Science: Natural Sciences and Technology 34, no. 1 (2018). http://dx.doi.org/10.25073/2588-1140/vnunst.4717.

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Dissolved oxygen (DO), total biomass and oxygen demand of nematode communities in the organic shrimp farms located in Tam Giang commune, Nam Can District, Ca Mau province were investigated in three seasons (March-dry, July-transfer and November-wet season) of 2015. The results showed that most of DO values were within permissible limits. However, the frequency distributions of DO values are very compressed at the lower limit of their scale. Total dry biomass varied from 24.77 to 937.04 µgC/10cm2 while oxygen demand ranged from 3467.39 to 64288.50 nlO2/day/10cm2. These values were slightly high

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