DOCSLIB.ORG

Constellation / Galaxie Copernicus Lowercase Romans

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Constellation / Galaxie Copernicus Lowercase Romans Constellation / Galaxie Copernicus Lowercase Romans 170pt 150pt zofia years 135pt VILLAGE xochie 120pt wanted 105pt voluntas WWW.VLLG.COM 1 Constellation / Galaxie Copernicus Lowercase Italics 170pt 150pt udon touze 135pt VILLAGE streak 120pt rubious 105pt quarrera WWW.VLLG.COM 2 Constellation / Galaxie Copernicus Uppercase Romans 170pt PINK 150pt OSLO 135pt VILLAGE NICHT 120pt MERLE 105pt LOGIUM WWW.VLLG.COM 3 Constellation / Galaxie Copernicus Uppercase Italics 170pt KIND 150pt JUMP 135pt VILLAGE IZORA 120pt HEADY 105pt GAMOW WWW.VLLG.COM 4 Constellation / Galaxie Copernicus All weights & styles Heavy & Heavy Italic 30pt ADVISOR BOUDICA congrued dexterity excerpts florence Bold & Bold Italic 30pt GENUINE HIGHBOY inworking jargoneer krantzes languets Medium & Medium Italic 30pt MAIGRES NOMINAL VILLAGE ostracods pomatoes quadding romanise Book & Book Italic 30pt SPELUNK TUNEFUL undernote vitaminise wrasting xiphogagi Light & Light Italic 30pt YIELDING ZESTFUL avisement breakeven celluloid dropshot WWW.VLLG.COM 5 Constellation / Galaxie Copernicus Sample Text Settings BOLD & BOLD ITALIC 10pt Polaris, designated Ursae Minoris (Latinized to Alpha Ursae Minoris, abbreviated Alpha UMi), commonly the North Star or Pole Star, is the brightest star in the constellation of Ursa Minor. It is very close to the north celestial pole, making it the current northern pole star. The revis ed Hipparcos parallax gives a distance to Polaris of about 433 light-years, while calculations by other methods derive distances around 30% closer. Polaris is a triple star system, compo sed of the primary star, Polaris Aa, in orbit with a smaller companion (Polaris Ab); the pair in orbit with Polaris B (discovered in August 1779 by William Herschel). There were once thought to be two more distant components—Polaris C and Polaris D—but these have been shown n ot to be physically associated with the Polaris system. Polaris Aa is a 5.4 solar mass F7 yell ow supergiant of spectral type Ib. It is the first classical Cepheid to have a mass determined from its orbit. MEDIUM & MEDIUM ITALIC 10pt Polaris B can be seen even with a modest telescope. William Herschel discovered the star i n August 1779 using a reflecting telescope of his own, one of the best telescopes of the time. B y examining the spectrum of Polaris A, it was also discovered in 1929 that it was a very close bi nary, with the secondary being a dwarf, which had been theorized in earlier observations. In Ja nuary 2006, NASA released images, from the Hubble telescope, that showed the three membe rs of the Polaris ternary system. Ab, the nearby dwarf star, is in an orbit of 18.5 AU from Polaris Aa, about the distance between the Sun and Uranus, which explains why its light is swamped b y its close and much brighter companion. Because Polaris lies nearly in a direct line with the Ea rth’s rotational axis above the North Pole—the north celestial pole—Polaris stands almost mo tionless in the sky, and all the stars of the northern sky appear to rotate around it. Therefore, it makes an excellent fixed point to draw measurements for celestial navigation. VILLAGE BOOK & BOOK ITALIC 10pt The moving of Polaris towards and, in the future, away from the celestial pole, is due to the pr ecession of the equinoxes. The celestial pole will move away from UMi after the 21st century, pas sing close by Gamma Cephei by about the 41st century, moving towards Deneb by about the 91s t century. The celestial pole was close to Thuban around 2750 BC, and during classical antiquity i t was closer to Kochab than to Polaris. It was about the same angular distance from UMi as to U Mi by the end of late antiquity. The Greek navigator Pytheas in ca. 320 BC described the celestia l pole as devoid of stars. However, as one of the brighter stars close to the celestial pole, Polaris was used for navigation at least from late antiquity, and described as “always visible” by Stobaeu s, and it could reasonably be described as stella polaris from about the High Middle Ages. In Sha kespeare’s play Julius Caesar, written around 1599, Caesar describes himself as being "as const ant as the northern star,” though in Caesar’s time there was no constant northern star. LIGHT & LIGHT ITALIC 10pt In the Hindu Puranas, it became personified under the name Dhruva. In the later medieval perio d, it became associated with the Marian title of Stella Maris “Star of the Sea” (so in Bartholomeus Anglicus, c. 1270s). An older English name, attested since the 14th century, is lodestar, cognate wi th the Old Norse leiðarstjarna, Middle High German leitsterne. The ancient name of the constella tion Ursa Minor, Cynosura, became associated with the pole star in particular by the early modern period. An explicit identification of Mary as stella maris with the polar star (Stella Polaris), as well as the use of Cyonsura as a name of the star, is evident in the title Cynosura seu Mariana Stella P olaris, a collection of Marian poetry published by Nicolaus Lucensis (Niccolo Barsotti de Lucca) in 1655. It was invoked as a symbol of steadfastness in poetry, as “steadfast star” by Spenser. Shak espeare’s sonnet 116 is an example of the symbolism of the north star as a guiding principle: “[Lov e]is the star to every wandering bark / Whose worth's unknown, although his height be taken.” WWW.VLLG.COM 6 Constellation / Galaxie Copernicus Sample Text Settings BOLD & BOLD ITALIC 8.5pt The Hipparcos spacecraft used stellar paralla on launched in 2013 and intended to measure s x to take measurements from 1989 and 1993 w tellar parallax to within 25 microarcseconds. Al ith the accuracy of 0.97 milliarcseconds, and it though it was originally planned to limit Gaia’s o obtained accurate measurements for stellar di bservations to stars fainter than magnitude 5. stances up to 1,000 pc away. The Hipparcos da 7, tests carried out during the commissioning p ta was examined again with more advanced err hase indicated that Gaia could autonomously id or correction and statistical techniques. Despi entify stars as bright as magnitude 3. When G te the advantages of Hipparcos astrometry, th aia entered regular scientific operations in July e uncertainty in its Polaris data has been point 2014, it was configured to routinely process sta ed out and some researchers have questioned rs in the magnitude range 3–20. Beyond that li the accuracy of Hipparcos when measuring bin mit, special procedures are used to download r ary Cepheids like Polaris. The Hipparcos reduct aw scanning data for the remaining 230 stars b ion specifically for Polaris has been re-examine righter than magnitude 3; methods to reduce a d and reaffirmed but there is still not widespre nd analyse these data are being developed; and ad agreement about the distance. The next ma it is expected that there will be “complete sky c jor step in high precision parallax measuremen overage at the bright end” with standard errors ts comes from Gaia, a space astrometry missio of “a few dozen Uas.” BOOK & BOOK ITALIC 8.5pt Ursa Minor, also known as the Little Bear, is a c an orange giant with an apparent magnitude of 2. onstellation in the Northern Sky. Like the Great B 08—only slightly fainter than Polaris. Kochab an ear, the tail of the Little Bear may also be seen as d magnitude 3 Gamma Ursae Minoris have been the handle of a ladle, hence the North American called the “guardians of the pole star.” Planets ha name, Little Dipper—seven stars with four in its ve been detected orbiting four of the stars, incl bowl like its partner the Big Dipper. It was one of uding Kochab. The constellation also contains an the 48 constellations listed by the 2nd-century isolated neutron star—Calvera—and H1504+6 astronomer Ptolemy, and remains one of the eig 5, the hottest white dwarf yet discovered, with a hty-eight modern constellations. Ursa Minor has surface temperature of 200,000 K. In the Babylo VILLAGE traditionally been important for navigation, part nian star catalogues, Ursa Minor was known as t icularly by mariners, because of Polaris being the he “Wagon of Heaven” (also associated with the North Star. Polaris, the brightest star in the const goddess Damkina). It is listed in the MUL.APIN c ellation, is a yellow-white supergiant and the brig atalogue, compiled around 1000 BC among the S htest Cepheid variable star in the night sky, rang tars of Enlil—that is, the northern sky. According ing from an apparent magnitude of 1.97 to 2.00. B to Diogenes Laërtius, citing Callimachus, Thales eta Ursae Minoris, also known as Kochab, is an a of Miletus “measured the stars of the Wagon by w ging star that has swollen and cooled to become hich the Phoenicians sail.” LIGHT & LIGHT ITALIC 8.5pt The tradition of naming the northern constellati as coined only in the early modern period. The an ons “bears” appears to be genuinely Greek, althou cient name of the constellation is Cynosura. The o ough Homer refers to just a single “bear.” The orig rigin of this name is unclear (Ursa Minor being a d inal “bear” is thus Ursa Major, and Ursa Minor was og’s tail would imply that another constellation ne admitted as second, or Phoenician Bear (Ursa Ph arby is the dog, but no such constellation is know oenicia, hence, Phoenice) only later, according to S n). Instead, the mythographic tradition of Cataste trabo (I.1.6, C3) due to a suggestion by Thales, who ismi makes Cynosura the name of an Oread nymp suggested it as a navigation aid to the Greeks, w h described as a nurse of Zeus, honoured by the g ho had been navigating by Ursa Major.
Load more

Recommended publications
  • Deep Optical Observations of Unusual Neutron Star Calvera with The
    to appear in The Astrophysical Journal Deep optical observations of unusual neutron star Calvera with the GTC† Yury Shibanov1,2, Andrey Danilenko1, Sergey Zharikov3, Peter Shternin1, Dima Zyuzin1 ABSTRACT Calvera is an unusual isolated neutron star with pure thermal X-ray spectrum typical for central compact objects in supernova remnants. On the other hand, its rotation period and spin-down rate are typical for ordinary rotation-powered pulsars. It was discovered and studied in X-rays and not yet detected in other spectral domains. We present deep optical imaging of the Calvera field obtained with the Gran Telescopio Canarias in g′ and i′ bands. Within ≈ 1′′ vicinity of Calvera, we detected two point-like objects invisible at previous shallow observations. However, accurate astrometry showed that none of them can be identified with the pulsar. We put new upper limits on its optical brightness of g′ > 27.87 and i′ > 26.84. We also reanalyzed all available archival X-ray data on Calvera. Comparison of the Calvera thermal emission parameters and upper limits on optical and non-thermal X-ray emission with respective data on rotation- powered pulsars shows that Calvera might belong to the class of ordinary middle-aged pulsars, if we assume that its distance is in the range of 1.5–5 kpc. Subject headings: stars: neutron – pulsars: general – pulsars: individual: Calvera, 1RXS J141256.0+792204, PSR J1412+7922 1. Introduction High Galactic latitude, b ≈ +37◦, compact source 1RXS J141256.0+792204 in the ROSAT All-Sky Survey was proposed as a neutron star (NS) candidate by Rutledge et al.
    [Show full text]
  • CONSTELLATION URSA MINOR, the LITTLE BEAR Ursa Minor
    CONSTELLATION URSA MINOR, THE LITTLE BEAR Ursa Minor (Latin: "Smaller She-Bear", to contrast with Ursa Major), also known as the Little Bear, is a constellation in the northern sky. Like the Great Bear, the tail of the Little Bear may also be seen as the handle of a ladle, hence the North American name, Little Dipper. It has seven main stars with four in its bowl, like its partner the Big Dipper. It was one of the 48 constellations listed by the 2nd-century astronomer Ptolemy, and remains one of the 88 modern constellations. Ursa Minor has traditionally been important for navigation, particularly by mariners, because of Polaris (at the end of the tail) being the North Star. Alpha Ursae Minoris, better known as Polaris, is the brightest star in the constellation, is a yellow-white supergiant and the brightest Cepheid variable star in the night sky, ranging from an apparent magnitude of 1.97 to 2.00. Beta Ursae Minoris, also known as Kochab, is an aging star that has swollen and cooled to become an orange giant with an apparent magnitude of 2.08, only slightly fainter than Polaris. Gamma Ursae Minoris, magnitude 3 and Kochab have been called the "guardians of the pole star". Planets have been detected orbiting four of the stars, including Kochab. The constellation also contains an isolated neutron star—Calvera—and H1504+65, the hottest white dwarf yet discovered, with a surface temperature of 200,000 K. HISTORY AND MYTHOLOGY In the Babylonian star catalogues, Ursa Minor was known as the Wagon of Heaven, Damkianna.
    [Show full text]
  • The Peculiar Isolated Neutron Star in the Carina Nebula Deep XMM-Newton and ESO-VLT Observations of 2XMM J104608.7-594306
    A&A 544, A17 (2012) Astronomy DOI: 10.1051/0004-6361/201219161 & c ESO 2012 Astrophysics The peculiar isolated neutron star in the Carina Nebula Deep XMM-Newton and ESO-VLT observations of 2XMM J104608.7-594306 A. M. Pires1,C.Motch2, R. Turolla3,4,A.Schwope1, M. Pilia5,A.Treves6,S.B.Popov7, and E. Janot-Pacheco8 1 Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany e-mail: [email protected] 2 CNRS, Université de Strasbourg, Observatoire Astronomique, 11 rue de l’Université, 67000 Strasbourg, France 3 Universitá di Padova, Dipartimento di Fisica e Astronomia, via Marzolo 8, 35131 Padova, Italy 4 Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey, RH5 6NT, UK 5 Netherlands Foundation for Research in Astronomy, Postbus 2, 7990 AA, Dwingeloo, The Netherlands 6 Universitá dell’Insubria, Dipartimento di Fisica e Matematica, via Valleggio 11, 22100 Como, Italy 7 Sternberg Astronomical Institute, Lomonosov Moscow State University, Universitetskii pr. 13, 119991 Moscow, Russia 8 Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, R. do Matão 1226, 05508-090 São Paulo, Brazil Received 2 March 2012 / Accepted 7 May 2012 ABSTRACT While fewer in number than the dominant rotation-powered radio pulsar population, peculiar classes of isolated neutron stars (INSs) – which include magnetars, the ROSAT-discovered “Magnificent Seven” (M7), rotating radio transients (RRATs), and central compact objects in supernova remnants (CCOs) – represent a key element in understanding the neutron star phenomenology. We report the results of an observational campaign to study the properties of the source 2XMM J104608.7-594306, a newly discovered thermally emitting INS.
    [Show full text]
  • Search for Gravitational Waves from a Nearby Neutron Star Using Barycentric Resampling
    Search for Gravitational Waves from a nearby neutron star using barycentric resampling Thesis by Pinkesh K. Patel In Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy California Institute of Technology Pasadena, California 2010 (Defended Aug 26, 2010) ii c 2010 Pinkesh K. Patel All rights Reserved iii To my Mum and Dad... iv Preface The work presented in this thesis was carried out within the LIGO Scientic Col- laboration (LSC). The methods and results presented here are under review and are potentially subject to change. The opinions expressed here are those of the author and not necessarily those of the LSC. The author gratefully acknowledges the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory, which provided support for this work. v Acknowledgements It is the memories that remain with you, even after one can’t remember the exact moment, the faces of the people involved or even the year in which they happened. How does one thank all the people involved in creating all the wonderful memories I have had in the past five years? If I miss someone, know that I will remember all the sweet or sour memories that I have shared with you. Sour memories also have their place and make me the person I am. So thank you all the people who thought they were unkind to me or said things I didnt want to hear. You also shaped me, just as much as the people I hold dear. I would like to start by thanking the California Institute of Technology, lov- ingly known as Caltech.
    [Show full text]
  • Central Compact Objects As Anti-Magnetars
    Central Compact Objects as Anti-magnetars Eric V. Gotthelf (Columbia University) with Jules P. Halpern & Rosalba Perna The Fast and the Furious ☀ 23 May 2013, Madrid, Spain Animation from Patnaude & Fesen 2009 Talk Outline • Properties of CCOs: a Class of Young NS • The CCO Pulsars Timing: the Anti-magnetars • Individual Anti-magnetars: Pulsars in SNRs Kes 79, 1E 1207.4-5209, Puppis A • Implications on the Formation and Evolution of CCOs • Where are the CCO descendants? • New results on Calvera, an new type of NS? • Implications and Future Work • Overview of Magnetic Fields and Neutron Star Evolution: Magnetic field structure (poloidal and toroidal); Anisotropic conductivity; Fallback / Buried field / Field decay? Distinguishing Properties of CCOs • Isolated NSs, • Near center of supernova remnants, • No optical or radio counterparts, • Lacking a pulsar wind nebula, • Steady, thermal X-ray emission, exclusively, • 2BB, kT ~ 0.3/0.6 keV; Lx ~ 1033 erg/s • (Don’t include NS in RCW 103: variable, 6h period) Central Compact Objects in Supernova Remnants Table 1: Central Compact Objects in Supernova Remnants a CCO SNR Age d P fp Bs Lx,bol 10 1 (kyr) (kpc) (ms) (%) (10 G) (erg s− ) RX J0822.0 4300 Puppis A 4.5 2.2 112 11 2.9 5.6 1033 − ⇥ 1E 1207.4 5209 PKS 1209 51/52 7 2.2 424 9 9.8 2.5 1033 − − ⇥ CXOU J185238.6+004020 Kes 79 7 7 105 64 3.1 5.3 1033 ⇥ CXOU J085201.4 461753 G266.1 1.2 1 1 . < 7 . 2.5 1032 − − ⇥ CXOU J160103.1 513353 G330.2+1.0 > 3 5 .
    [Show full text]
  • Grand Unification of Neutron Stars SPECIAL FEATURE
    Grand unification of neutron stars SPECIAL FEATURE Victoria M. Kaspi1 Department of Physics, McGill University, Montreal, QC, Canada H3A 2T8 Edited by Neta A. Bahcall, Princeton University, Princeton, NJ, and approved March 4, 2010 (received for review January 22, 2010) The last decade has shown us that the observational properties of emerged in the Chandra era. The isolated neutron stars (INSs; neutron stars are remarkably diverse. From magnetars to rotating poorly named because most RPPs are also isolated but are not radio transients, from radio pulsars to isolated neutron stars, from INSs) have as defining properties quasi-thermal x-ray emission central compact objects to millisecond pulsars, observational with relatively low x-ray luminosity, great proximity, lack of radio manifestations of neutron stars are surprisingly varied, with most counterpart, and relatively long periodicities (P ¼ 3–11 s). properties totally unpredicted. The challenge is to establish an Then there are the “drama queens” of the neutron-star popu- overarching physical theory of neutron stars and their birth proper- lation: the magnetars. Magnetars have as their true defining prop- ties that can explain this great diversity. Here I survey the disparate erties occasional huge outbursts of x-rays and soft-gamma rays, as neutron stars classes, describe their properties, and highlight well as luminosities in quiescence that are generally orders of results made possible by the Chandra X-Ray Observatory, in cele- magnitude greater than their spin-down luminosities. Magnetars bration of its 10th anniversary. Finally, I describe the current status are thought to be young, isolated neutron stars powered ulti- of efforts at physical “grand unification” of this wealth of observa- mately by the decay of a very large magnetic field.
    [Show full text]
  • XMM-Newton Eric Gotthelf (Columbia University)
    20 Years of Pulsar Observations with XMM-Newton Eric Gotthelf (Columbia University) • The X-ray Pulsar Population, • The XMM-Newton EPIC Instruments For Pulsar Measurements, • Compilation of XMM-Newton Pulsar Observations, • A Few of Many, Many Examples of XMM Pulsar Discoveries . XMM Timeline and Pulsar Science ASCA was the first broad-band (0.2-12 keV) spectro-imaging mission XMM fills a critical gap in time for broad-band pulsar studied Takes the torch from ASCA tempo-imaging… ASCA RXTE XMM-NEWTON CHANDRA SWIFT NUSTAR NICER 1999 2002 2005 2008 2011 2014 2017 2020 YEAR Pulsar timing torch is now passed to NuStar and NICER, But joint XMM and Chandra obs. provides a powerful new spectroscopic tool XMM Observations of Pulsars XMM-Newton’s timing and phase-resolved spectroscopy capabilities is well match for studying the characteristics of pulsars… The EPIC is the prime instrument for observing pulsars EPIC pn SmallWindow 5.7 ms resolution (4.3’x4.3’ FoV; 71% LiveTime) EPIC pn Timing 0.03 ms & MOS 1.5 ms (~1D Image; ~100% LiveTime) XMM EPIC Pulsar timing advantages Long, uninterrupted observations, large collection area Sub arcmin PSF, low energy response to 0.2-12 keV Minimum detectable pulsed fraction ~ f_p(min) ~ sqr(2S/N), N= total counts, S=signal power (FFT, Z^2_n) f_p(min) is increased by background counts N_b, as (1+N_b/N_s) Background included all unpulsed detected counts The X-ray Pulsar Population • RPPs: Rotation-Powered Pulsars (young/high Edot, Crab/Vela) • XINSs: X-ray Isolated Neutron Stars (Magnificent Seven) • CCOs: Central
    [Show full text]
  • Isolated Neutron Stars: Calvera and Beyond
    Isolated Neutron Stars: Calvera and Beyond Bob Rutledge McGill University Collaborators: Derek Fox and Andrew Shevchuk (PSU) Monica Turner (McGill) Jason Hessels, Ben Stappers X-ray Observations of Isolated Compact Objects • Isolated Compact Objects are presumably remnants of stellar evolution. • Isolated objects are unaffected by the evolution of a binary companion (such as in LMXBs), and they can provide a “pristine” look at the properties of “neutron stars” -- generically, the compact objects which are the result of supernovae at the end of a massive star’s H-burning lifetime. What is an “Isolated Neutron Star”, and what does it have to do with Gravity Waves? • Stellar Evolution gives ~ 109 neutron stars formed in supernovae in our galaxy over its history. Perhaps (?) 109 LIGO targets? Where are they all? • Isolated Neutron Stars (INSs) are an observationally defined class of compact object: • Discovered in the X-ray band (kT~50-600 eV). • Not a radio pulsar • No stellar companion (evidence: no, or little optical emission) • Summary: INSs result from detection of compact objects through thermal emission from their surface. INSs: Promising Gravitational Wave Sources? • Con: unlike LMXBs and radio pulsars, the spin periods are (in general) not measured initially (or at all). Thus detecting GWs from INSs is only better from a completely blind all-sky search, by having a direction. • Pro: We don’t have strong observational constraints on the birth magnetic field distibution of neutron stars. INSs are where the golden “gravitars” would be discovered . • Pro: Expected to be many of them (the entire NS population) and so they can be very nearby compared with LMXBs and other rare compact objects (aids detection of weak sources).
    [Show full text]
  • PDF of This Talk
    DiscoveringDiscovering X-rayX-ray BrightBright NeutronNeutron StarsStars forfor CurrentCurrent andand Next-GenerationNext-Generation ObservatoriesObservatories DerekDerek B.B. FoxFox AstronomyAstronomy && AstrophysicsAstrophysics PennPenn StateState UniversityUniversity Chandra X – Boston – 24 September 2009 Isolated Neutron Stars • “Isolated neutron stars” – Blackbody spectrum (dominant) – Peak in far-UV / soft X- ray – Cooling age < 1 Myr – Minimal X-ray variability – Not radio pulsars – No binary companions – No supernova remnant • Optically faint – most extreme fX/fopt objects known • Identified as ROSAT All- Sky Survey (Bright Source Catalog) X-ray sources without optical counterpart The Magnificent Seven • Seven isolated neutron stars discovered over 1996– 2001 • All BSC sources – Serendipity – Targeted survey work (RBS) – Positions refined with HRI • Intriguing targets for detailed study – X-ray bright – Nearby (two with parallax) – Atmospheres amenable to modeling • Ultimate goals: – Measure masses and radii – Constrain nuclear equation of state – Investigate possibility of persistent GW emission RXS J1856.5-3754 • Discovered by Fred Walter • Bright X-ray source in front of the Corona Australis molecular cloud • Must be close → Low luminosity • Optical counterpart discovered with HST (V=25.6 mag) • X-ray to optical flux ratio confirms neutron star nature • Subsequent HST programs to measure parallax and proper Ho et al. 2006 motion • Distance: ~160 pc • Featureless spectrum, modeled as magnetic hydrogen atmosphere • Slow X-ray
    [Show full text]
  • Calvera: a Low-Mass Strangeon Star Torqued by Debris Disk?
    Draft version October 3, 2017 Preprint typeset using LATEX style AASTeX6 v. 1.0 CALVERA: A LOW-MASS STRANGEON STAR TORQUED BY DEBRIS DISK? Yunyang Li School of Physics and State Key Laboratory of Nuclear Physics and Technology, Peking University, Beijing 100871, China Weiyang Wang School of Physics and State Key Laboratory of Nuclear Physics and Technology, Peking University, Beijing 100871, China Key Laboratory of Computational Astrophysics, National Astronomical Observatories, CAS, Beijing 100012, China and School of Astronomy and Space Sciences, University of Chinese Academy of Sciences, Beijing 100049, China Mingyu Ge Key Laboratory for Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China Xiongwei Liu School of Physics and Space Science, China West Normal University, Nanchong 637002, China Hao Tong School of Physics and Electronic Engineering, Guangzhou University, Guangzhou 510006, China Renxin Xu School of Physics and State Key Laboratory of Nuclear Physics and Technology, Peking University, Beijing 100871, China and Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China (Received Sep 19, 2017; Revised XXXX; Accepted XXXX) ABSTRACT Calvera is a 59 ms isolated pulsar, being unique due to its non-detection in radio, optical and gamma- rays but the purely thermal emission in soft X-rays. It is suggested that Calvera could be an ordinary middle-aged pulsar with significant magnetospheric activity at a large distance (Shibanov et al. 2016). arXiv:1709.07679v2 [astro-ph.HE] 30 Sep 2017 Alternatively, it is proposed in this paper that Calvera is a low-mass strangeon star with inactive magnetosphere (dead). In this scenario, we jointly fit the spectra obtained by the XMM-Newton Observatory and the Chandra X-ray Observatory with the strangeon star atmosphere model.
    [Show full text]
  • Constellation / Galaxie Polaris Condensed Uppercase Romans
    CONSTELLATION / GALAXIE POLARIS CONDENSED UPPERCASE ROMANS 170PT ZUNYI 150PT YUMEN 135PT VILLAGE XYLOMA 120PT WAXWING 105PT VESTMENTS WWW.VLLG.COM 1 CONSTELLATION / GALAXIE POLARIS CONDENSED UPPERCASE ITALICS 170PT ULTRA 150PT TRITON 135PT VILLAGE SIGLARE 120PT REEDBIRD 105PT QUANTITATE WWW.VLLG.COM 2 CONSTELLATION / GALAXIE POLARIS CONDENSED LOWERCASE ROMANS 170PT power 150PT oxnard 135PT VILLAGE numeric 120PT multipath 105PT lineamental WWW.VLLG.COM 3 CONSTELLATION / GALAXIE POLARIS CONDENSED LOWERCASE ITALICS 170PT kotow 150PT journal 135PT VILLAGE idoneity 120PT headlines 105PT grecianized WWW.VLLG.COM 4 CONSTELLATION / GALAXIE POLARIS CONDENSED ALL WEIGHTS & STYLES HEAVY & HEAVY ITALIC 30PT ADALINE BERMED catalyst debated BOLD & BOLD ITALIC 30PT EDIFIERS FIRMURA glabrous heliozoic MEDIUM & MEDIUM ITALIC 30PT IMMENSE JETSOMS VILLAGE klaxoned longueuil BOOK & BOOK ITALIC 30PT MATRICES NOSHERIE odalisque phonetist LIGHT & LIGHT ITALIC 30PT QUALTAGH RINGSIDER sentiment trekschuit WWW.VLLG.COM 5 CONSTELLATION / GALAXIE POLARIS CONDENSED SAMPLE TEXT SETTINGS BOLD & BOLD ITALIC 14PT Polaris, designated Ursae Minoris (Latinized to Alpha Ursae Minoris, abbreviated A lpha UMi), commonly the North Star or Pole Star, is the brightest star in the conste llation of Ursa Minor. It is very close to the north celestial pole, making it the curre nt northern pole star. The revised Hipparcos parallax gives a distance to Polaris of about 433 light-years, while calculations by other methods derive distances arou nd 30% closer. Polaris is a triple star system, composed of the primary star, Polar is Aa, in orbit with a smaller companion (Polaris Ab); the pair in orbit with Polaris B (discovered in August 1779 by William Herschel). There were once thought to be tw o more distant components—Polaris C and Polaris D—but these have been sho wn not to be physically associated with the Polaris system.
    [Show full text]
  • Discovery of an Isolated Compact Object at High Galactic Latitude
    ApJ, in press Discovery of an Isolated Compact Object at High Galactic Latitude R. E. Rutledge1, D. B. Fox2, & A. H. Shevchuk2 ABSTRACT We report discovery of a compact object at high Galactic latitude. The object was initially identified as a ROSAT All-Sky Survey Bright Source Cata- log X-ray source, 1RXS J141256.0+792204, statistically likely to possess a high X-ray to optical flux ratio. Further observations using Swift, Gemini-North, and the Chandra X-ray Observatory refined the source position and confirmed the absence of any optical counterpart to an X-ray to optical flux ratio of FX(0.1–2.4 keV)/FV > 8700 (3σ). Interpretation of 1RXS J141256.0+792204– which we have dubbed Calvera – as a typical X-ray-dim isolated neutron star would place it at z ≈ 5.1 kpc above the Galactic disk – in the Galactic halo – −1 implying that it either has an extreme space velocity (vz ∼> 5100kms ) or has failed to cool according to theoretical predictions. Interpretations as a persistent anomalous X-ray pulsar, or a “compact central object” present conflicts with these classes’ typical properties. We conclude the properties of Calvera are most consistent with those of a nearby (80 to 260 pc) radio pulsar, similar to the ra- dio millisecond pulsars of 47 Tuc, with further observations required to confirm this classification. If it is a millisecond pulsar, it has an X-ray flux equal to the X-ray brightest millisecond pulsar (and so is tied for highest flux); is the clos- est northern hemisphere millisecond pulsar; and is potentially the closest known millisecond pulsar in the sky, making it an interesting target for X-ray-study, a radio pulsar timing array, and LIGO.
    [Show full text]