DOCSLIB.ORG

Results of the Magnetical and Meteorological Observations Made

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Results of the Magnetical and Meteorological Observations Made ' &,/^>jMC 3 . ^ 3lv ^ *''^0Oi ^^^^^ ^ Royal Observatory, Greenwich, London. S.E. SIR, pubheation I beg to inform you that the on the opposite of the Royal 01)SLTvatory mcntioiicl page/A.^r been forwarded to you to sign and 1 beg to request you to be good enough and return the accompanying receipt.* I am, Sir, Your olicdient Servant, W. H. M. CHRISTIE, Atftnmomcv Tioyal. * Xon-compliance with this request will be interpreted intimation that similar works are not desired in future. hT '.^^V R E S U L r s OF THE MAGNETICAL AND METEOROLOGICAL OBSERVATIONS UADH AT THE ROYAL OBSEEVATOEY, GREENWICH, I N r H K Y E A R 1882: UNDER THE DIRECTION OF W. H. M. C H U I S T I E, M.A. E.R.S. ASTRONOMER ROYAL. PUBLISHED BY ORDER OE THE BOARD OE ADMIRALTY IN OBEDIENCE TO HER MAJESTY'S COMMAND. LONDON: PRINTED BY EYRE AND S P O T T I S W O ODE, PRTNTERS TO THE QUEEN'S MOST EXCELLENT MAJESTY. FOR HER M.AJESTY'S ST.\TIONERY OFFICE. 1884-. ] N 1) E X. PAOE INTRODUCTION. Personul Establishment and Arrangements Hi General Descrtptidn of the Buildings and Instruments in The Magnetical and Meteorological Observatori/ m Positions of the Instruments iv and v Subjects of Observation vi Magnetic Instruments. Upper Declination Magnet vi Its Suspension : Stand: Double Box : Collimator: and Theodolite vi and vii Its Collimation Error : Torsion Force of its Suspending Skein viii Determination of the reading of the Azimuthal Circle of the Theodolite corresponding to the Astronomical Meridian ix Method of Making and Reducing Observations for Magnetic DecUnatiun .... ix Lower Declination Magnet '•• General principle of Photographic Registration xi Arrangements for recording the Movements of the Declination Magnet xii Scale for measurement of Ordinates of the Photographic Curve xiii Horizontal Force Magnet xiv Magnet Carrier : Suspensioti Skein : Suspension Pulleys xiv Plane Mirror, Telescope, and Scale for Eye-observation xiv and xv Adjustment of the Magnet at; and xvi xviii Eye-observations .- Photographic Record xvii and Scale for measurement of Ordinates of the Photographic Curve xviii Temperature coefficient xviii Vertical Force Magnet xix Supporting frame. Carrier, and Knife-edge .... xix Plane Mirror, Telescope, and Scale for Eye-observation xix Time of Vibration in the Vertical and Horizontal Planes x.r Determination of the value of the Scale xxi Eye-observations : Photographic Record xxi Scale for measurement of Ordinates of the Photographic Curve xxii Temperature coefficient xxii Dip Instrument xxiii Deflexion Instrument xxir Ra 5625. Wt. 21369. C" 2] i T N T) E X. PAGE INTRODUCTION—conc/«rferf. Earth Current Apparatus xxvi Earth Connexions: Wire Circuits xxvi Arrangements for Photographic Ifegistration xxvii Magnetic Reductions xxvii Treatment of the Photographic Curves xrvii and xxviii Results in terms of Gairxs's Absolute Unit xxriii Magnetic Distiirhanees and Earth Currents x,rix Scale Values of the different Jifagnetic Elements, iind Comparatire Values for different Absolute Units xxx and xxri Notes referring to the Plates rxa-ii Meteorological Instruments. Standard Barometek xxa-iii Its Position: Diameter of Tnhe : Correction for Capillarity xxxiii Correction for Index Error : Comparison with Kew Standard ....... xxxiii Photographic Barometek xxociii Arrangements for Photographic Hegistration xxxiii Determination of the Scale xxmv Dry and Wet Bulb Thermometers xxxii-^ Revolving Frame : Standard Thermometer xxxiv and xxxi^ Corrections for Inflex Error xxxv Photographic Dry and Wet Bulb Thermometers rxn- Radiation Thermometers xxxvi Earth Thermometers xxxvi Osler's Anemometer xxxvii Methodof registering the Direction and Pressure of the Wind xx.rrii and .r.rxviii Its Rain-gauge xx.rrii Robinson's Anemometer xx.rriH Rain-Gadges x.n-ix Electrometer a/ Instrument employed : general description .1/ Method of collecting the Electricity of the Atmosphere xH System of Registration xli ^ Sunshine Instrument xlii J^.. Ozonometer xlii Meteorological Reductions .rim System of Reduction xliii the the Deduction of Temperature of Dew-Point, and of the degree of Humidity . .rliv Rainfall : Clouds and Weather : Electricity . xlv to xlvii Meteorological Averages xlvii Observations of Luminous Meteors xMii INDEX. PAGE RESULTS OF MAGNETICAL AND METEOROLOGICAL ORSERVATTONS IN TABULAR ARRANGEMENT :— Reduction of the Magnetic Observations ("O (iv) Table 1.—Mean Magnedc Declination West for each Astronomical Day (iv) the . Table II Monthly Means of Magnetic Declination West at each Hour of Day . of Magnetic Table III.—Mean Magnetic Declination in each Month West ; and excess (v) Declination above 17°, expressed as Westerly Force in terms of Gauss's Metrical Unit Table IV. Mean Horizontal Magnetic Force (diminished by a Constant) for each Astro- nomical Day '^) Table V.—Means of Readings of the Thermometer placed within the box inclosing the Horizontal Force Magnet, for each Astronomical Day (vi) Table VI.—Monthly Means of Horizontal Magnetic Force (diminished by a Constant) at each Hour of the Day (vi) Table VII.—Monthly Means of Readings of the Thermometer placed within the box (vii) inclosing the Horizontal Force Magnet at each of the ordinary Hours of observation . Table VIII.—Mean Horizontal Magnetic Force in each Month, uncorrected for Temperature, expressed in parts of the whole Horizontal Force (diminished by a Constant), and and Mean expressed in terms of Gauss's Metrical Unit (diminished by a Constant) ; H.F. Temperature for each Month (v") Table IX.—Mean Vertical Magnetic Force (diminished by a Constant) for each Astro- nomical Day (*'i) Table X. Means of Readings of the Thermometer placed within the box inclosing the Vertical Force Magnet for each Astronomical Day (viii) Table XI. Monthly Means of Vertical Magnetic, Force (diminished by a Constant) at each Hour of the Day C^) Table XII.—Monthly Means of Readings of the Thermometer placed within the box in- closing the Vertical Force Magnet at each of the ordinary Hours of observation . (ix) Table XIII.—Mean Vertical Magnetic Force in each Month, uncorrected for Temperature, expressed in parts of the whole Vertical Force (diminished by a Constant), and expressed in terms of Gauss's Metrical Unit (diminished by a Constant) ; and Mean V.F. Temperatui-e for each Month (x) Table XJV Mean Diurnal Inequalities of Declination, Horizontal Force, and Vertical Force for the year (*>) "^ Table XV.—Diurnal Range of Declination and Horizontal Force as deduced from the Twenty-four Hourly Measures of Ordinates of the Photographic Register on each day (xii) (xii) Table XVI.—Monthly Mean Diurnal Eange of Declination and Horizontal Force . , . Results of Observations of the Magnetic Dip (xiii) Dips observed (^i^) Monthly Means of Magnetic Dips (xvi) ,xvii) Yearly Means of Magnetic Dips, and General Mean - . — RESULTS OF MAGNKTICAL AND MKTEOROLOGTCAI. OBSKRVA TTONS— rrt«/;,n/r,/. OliSERVATlOXS OF DEFLEXION OF A MaGNF.T FOR AbSOI-UTK Mf.ASURF. OF IIORIZOXTAI. Force (xix) Abstract of the Observations of Deflexion of a Magnet, ami of Vibrations of tho Deflectinj; Magnet for Absolute Measure of Horizontal Force (,xx) Computation of the Values of Absolute Measure of Horizontal Forrp (xxi) Magn-etic DisTURnANOES AND Earth CiRRENr- (xxiii) I'rief description of Magnetic Movements (superposed on the ordinary diurnal movement) exceeding o' in Declination, ()-0015 in Horizontal Force, or 0-0005 in Vertical Force, taken from the Pliotograpliic Registei' (xxiv) Explanation of tlie Plates of Magnetic Disturbances .and Earth Currents (xxviii) Pr.ATKS I. TO XXII, photo-lithographed from tracings of the Photographic IJegisleis uf Miitr- netic Disturbances and Earth Currents. Results of Meteorological Obseuvation-s (xxixj Daily Results of Meteorological Observations (xxx) Highest and Lowest Readings of the Barometer (liv) Absolute Maxima and Minima Readings of the Haromoter for each .Month (Ivi') Monthly Results of Meteorological Elements flvii) Monthly Mean Reading of the Barometer at ex cry I Iniii- (, I' ihf D.iy (Iviii) Monthly Mean Temperature of the Air at every Hour of the Day (Iviii) Monthly Mean Temperature of Evaporation at every Hour of the Day (lix) Monthly Mean Temperature of the Dew- Point at every Hour of the Day (lix^ ^ Monthly Mean Degree of Humidity at every Hour of the Day (Ix) rt A..-4-%^^_^ J Total Amount of Sunshine registered in each Hour of the Day ill each nioiitli .... (Ix) Kiirtli Theniioraclers : • ( 1 .) Reading of a Thermometer whose bulb is sunk to the depth of 25 ti feet (24 French feet) below the surface of the soil, at Noon on every Day (Ixi) (II.) Readingof a Thermometer whose bulb is sunk to the depth of 12-8 feet (12 French feet) below the surface of the soil, at Noon on every Day dxi) (HI.) Reading of a Thermometer whose bulb is sunk to the depth of 6'4 feet (G Frencli feet) below the surface of the soil, at Noou ou every Day (Ix'i) (IV.) Reading of a Thermometer whose bulb is .sunk to the depth of 3 '2 feet (3 French feet) below the surface of the soil, at Noon ou every Day (Ixiii) (V.) Reading of a Thermometer whose bulli is sunk to the dejith of 1 inoli below .ie surface of the soil, at Noon on every Day (Ixiv) (VI.) Reading of a Thermometer within the case covering the Deep-sunk Theiinometers, whose bulb is placed on a level with their scales, at Noon ou every Day . ( Ixv) Abstract of the Changes of the Direction of the Wind, as derived fi'om the Records of Osier's Anemometer (Ixvi) Mean Hourly Measures of the Horizontal Movement of the Air in each Month, and Greatest and Least Hourly Measures, as
Load more

Recommended publications
  • 物理雙月刊29-3 621-772.Pdf
    ᒳृݧ ʳ ౨ᄭઝݾറᙀ ᚮࣔᏕ/֮ Δࢨუ෡Եᛵᇞݺଚشଶಬߨጿጿլឰऱਞ ၦऱࠌ ౨ᄭऱ࿨࣠Δኙ٤෺شॸΔ᠏ณհၴԾࠩԱքΕԮִ መ৫ࠌ ഏᎾၴऱڇऱᐙ᥼ګԳพஒऱ ᛩቼࢬທח᥆࣍ङ୙ऱֲ՗Δ עء۶Δլ݋ោᥦԫՀڕټ᦭ᚰۖࠐΖ ඈچᑷ௡ԫंंլឰ ᨜Δᑷ௡ รԼᒧറ֮ΚψൕഏᎾᛩቼਐᑇ؀؄ࡌ੡௧੉ᛩ៥ऱ ᨜ऱ࿇ሽ౨ᄭ؀ऱᛘ௛Δ ֗ IEA อૠ઎װ൅ထԫैཀհլ݈ ωΔᇠᒧ֮ີტ᝔խᘋՕᖂ܉᨜ऱՕ௛հխΔᨃԳ ։؀ᗺ៥࣍ ᤚ൓ຑ़௛Εຑ௧੉ຟ૞आᤴ ढ෻ߓ୪ւࣳඒ඄࣍ඒᖂઔߒ խࢼ़੡ݺଚᐷᐊΖڦۍऱ ؀Ꭹ୙հᎾΔڼԱΖՈࠌ൓ଖ ᆖᛎࡉഏԺऱ࿇୶זᆏᆏՂ ෼چሽլឰش୽ڞ᨜ऱ ᎅ࠷ެ࣍౨ᄭױሽ ፖ๵ᑓΔ༓׏شڇΔኚ໌೏୽ΖྥۖΔ֒ Δޡݾ๬ऱၞشࠡሎ֗شழΔݺଚՈ੡Օ௛ ऱࠌٵ೏୽ཚऱ ᎅਢԫഏᆖᛎ࿇୶ऱ଺ױCO2 ऱඈ࣋ၦࡉ׈੺ᄵ৛யᚨ ౨ᄭ ٺΔ౨ᄭᤜᠲኙ࣍ڼڂऱ༞֏ΔထኔఎՀԱլ֟լߜ ೯ԺΖ ࡳࢤެڶᏆ഑ऱ࿇୶ࠠٺڇ෺ᄊ֏ ഏچຒףԱګऱધᙕΔՈ ߪᣂএࠩԫ౳षᄎՕฒऱ壂ઘࡉֲൄढ֊ޓயᚨऱ׌૞ං֫հԫΖ ऱᐙ᥼Δ ฒاڇवኙ࣍ Ꮭऱं೯ΖᅝഏᎾईᏝՂཆΔഏփढᏝঁஓஓױݺଚ੡ࠆ࠹ԫաऱ堚ළፖঁ൸հᎾΔڇ ՂይΖچ᨜Δ ऱ঩ৼᜢխᆥྤݲᐫ؀ᇷᄭᤖ៲ຆ׎Δ౨ᄭ༓׏٤ᑇٛᘸၞՑऱྥ֚ 9 ڣ ࣍ 2005ޓࠐΔ׈੺ईᏝᆏᆏ֒೏Δڣၦথբ २༓شࢬ௣౛ऱؓ݁ሽၦࡉ౨ᄭࠌڣޢԳޢݺଚ ද೏࣍ US$70 ऱ໌ޢࠐऱᖵ׾ᄅ೏Δሒڣۍሽ ִٝડధڇ౨ᄭΕڇ᨜؀׈੺ऱছૄΜૉ൞უ઎઎ڇټਢඈ ᄭ۞ᖏञࡉైڂຝ։ڶᄅ೏ધᙕΖ׈੺ईᏝऱं೯ឈ ᚮࣔᏕ ౨ᄭف෺Ղ֏چլ؆׏ਢڂ׼ԫ׌૞଺܀ਙएࠃٙΔ 堚ဎՕᖂढ෻ߓمഏ ڶईΕ֚ྥ௛ࡉᅁ࿛౨ᄭᗏற)ऱᤖ៲ၦึߒفऑਐ) E-mail: [email protected] ฾ࢤΔ׊ૉشऱ౨ᄭࠌڶૻΖറ୮ေ۷ૉ௅ᖕԳᣊ෼ Ϯ621Ϯʳ քִʳڣ ˊ˃˃˅ʻ֥԰࠴Կཚʼʳעढ෻ᠨִ ᒳृݧ ༚ྼऱ᝟ႨΖᅝᓫᓵᇠ֘ுΛࢨਢᇠᖑுΛംᠲڶۖ ࠩބயऱᆏ౨ֱூΔࢨլᕣݶ༈ڶإటנ༼౨آᙈᙈ ෻ᇞு౨ᗏறऱ፹ທመچհছΔषᄎՕฒᚨᇠ٣堚ᄑ ڶ෺Ղೈᅁᇷᄭࡸچ౨ᄭऱᇩΔঞזࠠ೏ய෷հཙ ਩؆ਜ਼ழऱۆுᘿ୴֗א଺෻Δ܂࿓ࡉு౨࿇ሽऱՠ فईࡉ֚ྥ௛࿛֏فڕהऱᤖ៲ၦ؆Δࠡ׳ؐڣ 200 ෻ࢤড়ᨠऱኪ৫੡אթ౨ڼڕୌࠄΔڶՂऱ׈੺ ߻ᥨൻਜࠩࢍאڣ ౨ྤऄ֭ᐶመ 50ױၦቃ۷ژᗏறऱᚏ ཚ௽ءΔڼڂᖗΖހᒔऱإԫנு౨࿇ሽ೚شࠌܡၦΖ ਢޣ౨ᄭ᜔Ꮑ ሽֆ׹ுԿᐗૠቤิ९೏ದ໑Փऱᑷ֧֨؀ᗏ ܑຘመف׊᠏ངய෷ለ೏հႚอ֏܅ءګΔᆖᛎۖྥ ሽֆ׹ு౨࿇ሽ؀ኔ೭ᆖ᧭ऱڣڍڶࠩԱٍࠠބऱሽ౨ ៺Δشऴ൷ࠌאԫ౳Օฒ൓ګ᠏ངڇΔشறऱࠌ ،੡ݺଚ੡֮റ૪ψࢢسࢨᑷ౨ऱመ࿓խΔᄎ ๠ு֨ᛜሎᓰᓰ९׆ᐚᆠ٣(شԺ࿇ሽ)Ε೯౨(ሎᙁ־อጠ) ॺൄ෍᧩࣐ᚩऱאԱᇞ،--ு౨࿇ሽ෍ᓫωΔᇠ֮ڕլ ۆᎨॸΔᖄીᣤૹऱᛩቼګඈ࣋Օၦऱᄵ৛௛᧯ࡉݮ ຝ๠෻ٺᎅࣔԱு౨࿇ሽऱچ੡ᦰृ堚ᄑڗ෺ऱؓ݁ᄵ৫ 壄᥸֮چ਩ࡉֲ᝟ᣤૹऱᄵ৛யᚨΔၞۖᖄી ኪؓᘝ ੌ࿓ࡉுᗏறՄऱ፹ທመ࿓Δਢԫᒧॺൄଖ൓ԫᦰऱسऱڶ෺ऱ۞ྥᛩቼࡉ଺چኙۖڂດዬՂ֒Ζ ኪᛩቼ૿ ֮ີΖس෺ऱچऱᣤૹᓢᚰΔࠌڃனױլګؘലທ ٤ᤜᠲǵഏᎾ଺ईᏝ௑ࡺ೏լڜईفᜯ؎ՕऱਗᖏΖ ࠹ࠩ٤෺ ՂഏᎾၴ๵ᒤᄵ৛௛᧯ඈ࣋྇ၦࢭᘭհᛩঅֆףࡉ௛ଢऱ᧢ᔢࢬທ ՀΔ᧢ޏኙᛩቼऱشᣂ౨ᄭሎڶ ڂᛩঅრᢝ೏ይ࿛֗אඔ೯Δڤإऱᐙ᥼ຍଡૹ૞ᤜᠲΔݺଚ௽ܑࡡᓮՠᄐݾ๬ઔߒ પψࠇຟᤜࡳ஼ωګ ੡ԳᣊؘߨհሁΖ۶ᘯګ౨ᄭسᡖᐚ ైऱᓢᚰՀΔං೯٦ۂ(Հ១ጠՠઔೃ౨ᛩࢬא)ೃ౨ᄭፖᛩቼઔߒࢬ ౨ᄭ࿇ሽωٍ௽ᆖسรքᒧറ֮ψ٦עء౨ᄭΛس٦
    [Show full text]
  • Physical Processes in the Interstellar Medium
    Physical Processes in the Interstellar Medium Ralf S. Klessen and Simon C. O. Glover Abstract Interstellar space is filled with a dilute mixture of charged particles, atoms, molecules and dust grains, called the interstellar medium (ISM). Understand- ing its physical properties and dynamical behavior is of pivotal importance to many areas of astronomy and astrophysics. Galaxy formation and evolu- tion, the formation of stars, cosmic nucleosynthesis, the origin of large com- plex, prebiotic molecules and the abundance, structure and growth of dust grains which constitute the fundamental building blocks of planets, all these processes are intimately coupled to the physics of the interstellar medium. However, despite its importance, its structure and evolution is still not fully understood. Observations reveal that the interstellar medium is highly tur- bulent, consists of different chemical phases, and is characterized by complex structure on all resolvable spatial and temporal scales. Our current numerical and theoretical models describe it as a strongly coupled system that is far from equilibrium and where the different components are intricately linked to- gether by complex feedback loops. Describing the interstellar medium is truly a multi-scale and multi-physics problem. In these lecture notes we introduce the microphysics necessary to better understand the interstellar medium. We review the relations between large-scale and small-scale dynamics, we con- sider turbulence as one of the key drivers of galactic evolution, and we review the physical processes that lead to the formation of dense molecular clouds and that govern stellar birth in their interior. Universität Heidelberg, Zentrum für Astronomie, Institut für Theoretische Astrophysik, Albert-Ueberle-Straße 2, 69120 Heidelberg, Germany e-mail: [email protected], [email protected] 1 Contents Physical Processes in the Interstellar Medium ...............
    [Show full text]
  • Oregon Star Party Advanced Observing List
    Welcome to the OSP Advanced Observing List In a sincere attempt to lure more of you into trying the Advanced List, each object has a page telling you what it is, why it’s interesting to observe, and the minimum size telescope you might need to see it. I’ve included coordinates, the constellation each object is located in, and either a chart or photo (or both) showing what the object looks like and how it’s situated in the sky. All you have to do is observe and enjoy the challenge. Stretch your skill and imagination - see something new, something unimaginably old, something unexpected Even though this is a challenging list, you don’t need 20 years of observing experience or a 20 inch telescope to be successful – although in some cases that will help. The only way to see these cool objects for yourself is to give them a go. Howard Banich, The minimum aperture listed for each object is a rough estimate. The idea is to Chuck Dethloff and show approximately what size telescope might be needed to successfully observe Matt Vartanian that particular object. The range is 3 to 28 inches. collaborated on this The visibility of each object assumes decently good OSP observing conditions. year’s list. Requirements to receive a certificate 1. There are 14 objects to choose from. Descriptive notes and/or sketches that clearly show you observed 10 objects are needed to receive the observing certificate. For instance, you can mark up these photos and charts with lines and arrows, and add a few notes describing what you saw.
    [Show full text]
  • OCTOBER 2009 OBSERVER Inside the the Chill’S A-Comin’ Observer
    THE DENVER OBSERVER OCTOBER 2009 OBSERVER Inside the The Chill’s a-Comin’ Observer President’s Corner........................... 2 Society Directory............................. 2 Prelude Lake................................... 3 New Scope Operator......................... 5 New Members.................................. 5 Astronomical League....................... 6 NASA’S Space Place......................... 7 Schedule of Events.............. back page Calendar 4.................................................... Full moon BUT NOWHERE NEAR THE TEMPERATURE INSIDE THE MU CEPHEI NEBULA 11..................................... Last quarter moon CLOUD, IC 1396 IN CEPHEUS, WHERE A FRIGID -290ᵒ AWAITS A STELLAR ADVENTURER 17.................................................. New moon Joe used an SBIG ST-2000XM ccd camera with a 110mm Mamiya RZ lens at f/5.6. Please contact Joe for more technical details. The bright orange star is Mu Cephei, the Garnet Star; 24........................ Colorado Astronomy Day the Elephant Trunk nebula portion is right of center. 25.................................... First quarter moon Image copyright 2009 Joe Gafford OCTOBER SKIES by Dennis Cochran upiter is already up in the south when darkness descends, situated along Alpha Aquarius, the star at the top of the arc of that constellation. Above it J the top left of Capricornus’ goat-ee jester grin. Above Jupiter and the a short way and a bit west is the slightly brighter red star, Enif, at the end of Goat is the water jug of Aquarius, in case you’ve ever wondered where one of Pegasus’ legs. Just northwest of Enif is M15, one of the best globulars this elusive constellation lies. Wasn’t there an Age of Aquarius? Perhaps that on the list. If you then drop from Enif or M15, straight south about 2/3 of was when the New Age movement was born.
    [Show full text]
  • Chromospheric Activity Induced by Short-Period Planets a Search for Modulation of Ca II H &; K Emission
    Chromospheric Activity Induced by Short-Period Planets A Search for Modulation of Ca II H &; K Emission by Evgenya Shkolnik B.Sc. (Physics and Mathematics), Dalhousie University, 1998 M.Sc. (Astronomy), The University of British Columbia, 2000 A THESIS SUBMITTED IN PARTIAL FULFILMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY in The Faculty of Graduate Studies (Department of Physics and Astronomy) We accept this thesis as conforming to the required standard THE UNIVERSITY OF BRITISH COLUMBIA December 4, 2003 © Evgenya Shkolnik, 2003 Abstract I have detected the first evidence of magnetic interaction between an extra- solar planet and its parent star. Of the > 100 extrasolar planets discovered to date, approximated 20% of them are '51 Peg'-type with a Jupiter-mass planet orbiting within 0.1 As- tronomical Units. The systems with the tightest orbits (P orb < 5 days) offer the best opportunity to observe a tidal or magnetic interaction between the planet and its parent star. Stellar chromospheric activity could be modu- lated in two ways. For magnetic interaction, the modulation is predicted to be at the orbital period with enhancement near the sub-planetary point (</> = 0). Tidal interaction would stimulate activity with a period of Porb/2 with enhancements near both <j> — 0 and 0.5. The Ca II H & K line reversals at 3968 and 3933 A are the best chro- mospheric activity indicators visible from the ground. I observed the H & K emission cores of five sun-like stars with short period planets: r Boo, HD179949, HD 209458, 51 Peg and v And.
    [Show full text]
  • The Observer
    The Observer The Official Publication of the Lehigh Valley Amateur Astronomical Society https://lvaas.org/ https://www.facebook.com/lvaas.astro September, 2019 Volume 59 Issue 09 1 The Elephant Trunk nebula in constellation Cepheus, imaged in narrowband (H alpha, SII, and OIII); 10 minute exposures (30 frames of H alpha, 16 frames O3, 17 frames S3) for just over 10 hours cumulative exposure time. I processed in DSS and photoshop and used a modified Hubble palette (SHO) where green is changed to a more pleasing gold color. Imaged by Jason Zicherman. Cover image: The Dumbbell nebula by Jason Zicherman Date of acquisition: 7/11,7/13,7/20, 2019; H alpha 600 second exposures x 10; luminosity 300 seconds exposure x 15, RGB 300 seconds x 15 each; processed in Deep sky stacker and Photoshop; Acquired with Sequence Generator Pro and PHD2; H alpha data was layered on top of LRGB as an additional Luminosity layer. Tec 140 f7 scope on Astrophysics 1100 Goto mount, TEC 0.9x flattener/reducer. Camera: QSI 685 wsg; Astrodon filters, off axis guider: Ultrastar 2 ad ast ra*********************************************** Have you visited Pulpit Rock lately (or ever)? If not, you are missing out on one of the greatest benefits of LVAAS membership. We will all probably remember this summer for the excessive rain that we experienced in the beginning of the season, and the record-breaking heat in July, but let's also remember the really fine evenings we had for several LVAAS events on the mountain. M eg a M eet We only needed to reschedule Mega Meet once this year, but the revised date crept up and surprised me.
    [Show full text]
  • Annual Report 2003
    Deutsches Zentrum für Luft- und Raumfahrt e.V. German Aerospace Center Institute of Planetary Research SECTION: “PHYSICS OF SMALL BODIES AND EXTRA-SOLAR PLANETS” Annual Report 2003 OBSERVATIONS MODELLIN G FIREWATCH TECHNOLOGY SPACE MISSIONS http://solarsystem.dlr.de/KK 0 From left to right: First row: Detlef de Niem [email protected] Scientific staff member Dr. Alan W. Harris [email protected] Deputy section leader Dr. Anders Erikson1 [email protected] Scientific staff member Dr. Carmen Tornow [email protected] Scientific staff member Second row: Holger Voss1 [email protected] PhD student Dr. Gerhard Hahn [email protected] Scientific staff member Prof. U. Motschmann [email protected] Guest scientist Dr. Heike Rauer1 [email protected] Group leader Dr. Ekkehard Kührt [email protected] Section leader Dr. Jörg Knollenberg [email protected] Scientific staff member Rosemarie Mooseder Secretary (retired) Michael Müller [email protected] PhD student Martin Prescher Guest student Egon Braatz [email protected] Technical staff member Not appearing in the photo: Dr. Stefano Mottola [email protected] Scientific staff member Ralph Kahle [email protected] PhD student Michael Weiler 1 [email protected] PhD student Stephanie Werner [email protected] PhD student 1 Group: Extrasolar planets and cometary atmospheres 1 Contents Contents................................................................................................................................ 2 1. Introduction (E. Kührt)....................................................................................................... 3 2. Asteroid science................................................................................................................ 4 2.1 Keck thermal-infrared observations of near-Earth asteroids (A. W. Harris)..................... 4 2.2 Investigations of the physical properties of near-Earth asteroids with data from the NASA Infrared Telescope Facility (A.
    [Show full text]
  • October 2020 BRAS Newsletter
    A Neowise Comet 2020, photo by Ralf Rohner of Skypointer Photography Monthly Meeting October 12th at 7:00 PM, via Jitsi (Monthly meetings are on 2nd Mondays at Highland Road Park Observatory, temporarily during quarantine at meet.jit.si/BRASMeets). GUEST SPEAKER: Tom Field, President of Field Tested Systems and Contributing Editor for Sky & Telescope Magazine. His presentation is on Astronomical Spectra. What's In This Issue? President’s Message Secretary's Summary Business Meeting Minutes Outreach Report Asteroid and Comet News Light Pollution Committee Report Globe at Night Astro-Photos by BRAS Members Messages from the HRPO REMOTE DISCUSSION Solar Viewing Great Martian Opposition Uranian Opposition Lunar Halloween Party Edge of Night Observing Notes: Cepheus – The King Like this newsletter? See PAST ISSUES online back to 2009 Visit us on Facebook – Baton Rouge Astronomical Society BRAS YouTube Channel Baton Rouge Astronomical Society Newsletter, Night Visions Page 2 of 27 October 2020 President’s Message Happy October. I hope everybody has been enjoying this early cool front and the taste of fall that comes with it. More to our interests, I hope everybody has been enjoying the longer evenings thanks to our entering Fall. Soon, those nights will start even earlier as Daylight Savings time finally ends for the year— unfortunately, it may be the last Standard Time for some time. Legislation passed over the summer will mandate Louisiana doing away with Standard time if federal law allows, and a bill making it’s way through the US senate right not aims to do just that: so, if you prefer earlier sunsets, take the time to write your congressmen before it’s too late.
    [Show full text]
  • Fixed Stars Interview with Diana K. Rosenberg by Edith Hathaway, USA
    Fixed Stars Interview with Diana K. Rosenberg By Edith Hathaway, USA ob Hand calls Diana K. Rosenberg “the leading authority on Fixed Stars.” She has spent the past 30 years researching the subject of Fixed Stars. Her primary interest R has always been research and teaching, rather than the consulting side of astrology. Her preferred astrological techniques outside of the realm of Fixed Stars include Uranian Astrology (90 Degree Dial, Planetary Pictures, etc.), Derived Houses, Planetary Nodes, and Solstice Points. Diana has been a resident of New York City her entire life, while my residence in NYC spanned only 7 years, and I moved westwards in the USA in Feb. 1983. Our paths first crossed in 1982 when I was a student in Diana’s Uranian Astrology classes in Manhattan, NY. From 1988 to the early 1990s I made a gradual shift from Uranian (tropical) to Vedic (sidereal) astrology, a subject Diana always intended to study, but Fixed Stars came to take up all of her time. She has always been fascinated with very ancient things, and the study of antiquity. A different portion of this interview, mainly on Fixed Stars, is being published simultaneously by ISAR Journal (Journal of the International Society for Astrological Research), both print and On-line versions. See http://www.isarastrology.com. This larger interview at Saptarishis covers only a few pages of the same material, but also much more from Diana on stars. It segues at times into a dialogue between us about Fixed stars, mundane astrology, the Vedic nakshatras, and the two zodiacs – tropical and sidereal (items #12 through 14), also about her life and birth chart, including my commentary on her Vedic chart, at her request (item #16).
    [Show full text]
  • NGC-7023 (Caldwell 4) (LBN 487) the Iris Nebula in Cepheus Introduction the Purpose of the Observer’S Challenge Is to Encourage the Pursuit of Visual Observing
    MONTHLY OBSERVER’S CHALLENGE Las Vegas Astronomical Society Compiled by: Roger Ivester, Boiling Springs, North Carolina & Fred Rayworth, Las Vegas, Nevada With special assistance from: Rob Lambert, Las Vegas, Nevada October 2012 NGC-7023 (Caldwell 4) (LBN 487) The Iris Nebula in Cepheus Introduction The purpose of the observer’s challenge is to encourage the pursuit of visual observing. It is open to everyone that is interested, and if you are able to contribute notes, drawings, or photographs, we will be happy to include them in our monthly summary. Observing is not only a pleasure, but an art. With the main focus of amateur astronomy on astrophotography, many times people tend to forget how it was in the days before cameras, clock drives, and GOTO. Astronomy depended on what was seen through the eyepiece. Not only did it satisfy an innate curiosity, but it allowed the first astronomers to discover the beauty and the wonderment of the night sky. Before photography, all observations depended on what the astronomer saw in the eyepiece, and how they recorded their observations. This was done through notes and drawings and that is the tradition we are stressing in the observers challenge. By combining our visual observations with our drawings, and sometimes, astrophotography (from those with the equipment and talent to do so), we get a unique understanding of what it is like to look through an eyepiece, and to see what is really there. The hope is that you will read through these notes and become inspired to take more time at the eyepiece studying each object, and looking for those subtle details that you might never have noticed before.
    [Show full text]
  • Small Wonders: Quick Peeks – Cepheus Tom Trusock – 10 / 08
    Small Wonders: Quick Peeks – Cepheus Tom Trusock – 10 / 08 Small Wonders: Quick Peeks - Cepheus Tom Trusock 10/08 Whaddya mean you can't see a king? Here's the king, his wife and their pet lizard too. Well, his head anyway. High overhead in the autumn sky lies one of the most impressive stars and star forming regions in the galaxy. Both are located in the constellation of Cepheus (the king) which is bordered by Cygnus and Cassiopeia (among others). Cepheus is relatively easy to locate with it's brightest stars forming a the rather distinctive shape of a child's house. To the south of Cepheus, we find the huge stellar nursery IC 1396. At around 2.5 deg by just over 2 deg, this HII region is one of the largest star forming regions in the night sky and occupies around 16 times the area of the full moon. IC 1396 lies some 3000 light years from your backyard - and perhaps only slightly further from mine ;) - on any given night and contains a number of targets in it's own right. This area is packed with deep sky objects. You'll find the Elephant's Trunk Nebula (IC 1396a), the open cluster Trumpler 37, the dark nebulae B161, B367, B163, B162, B160, and B365, various multiple stars, and perhaps most impressive of all, Herschel's Garnet Star - the Variable Mu Cephei - in the region. - 1 - Small Wonders: Quick Peeks – Cepheus Tom Trusock – 10 / 08 Wide field Finder Chart, Facing North - about 9:30pm Early October Targets of Interest - 2 - Small Wonders: Quick Peeks – Cepheus Tom Trusock – 10 / 08 And speaking of Mu, that's a good place to start.
    [Show full text]
  • Star Forming Regions in Cepheus
    Handbook of Star Forming Regions Vol. I Astronomical Society of the Pacific, 2008 Bo Reipurth, ed. Star Forming Regions in Cepheus M´aria Kun Konkoly Observatory, H-1525 Budapest, P.O. Box 67, Hungary Zolt´an T. Kiss Baja Astronomical Observatory, P.O. Box 766, H-6500 Baja, Hungary Zolt´an Balog1 Steward Observatory, University of Arizona, 933 N. Cherry Av., Tucson AZ 85721, USA Abstract. The northern Milky Way in the constellation of Cepheus (100◦ ≤ l ≤ 120◦;0◦ ≤ b ≤ 20◦) contains several star forming regions. The molecular clouds of the Cepheus Flare region at b > 10◦, are sites of low and intermediate mass star for- mation located between 200 and 450 pc from the Sun. Three nearby OB associations, Cep OB2, Cep OB3, Cep OB4, located at 600–800 pc, are each involved in forming stars, like the well known high mass star forming region S140 at 900 pc. The reflection nebula NGC7129 around 1 kpc harbors young, compact clusters of low and intermedi- ate mass stars. The giant star forming complex NGC7538 and the young open cluster NGC7380, associated with the Perseus arm, are located at d> 2 kpc. 1. Overview In this chapter we describe the star forming regions of the constellation of Cepheus. A large scale map of the constellation, with the boundaries defined by IAU overlaid, and the most prominent star forming regions indicated, is shown in Fig. 1. This huge area of the sky, stretching between the Galactic latitudes of about 0◦ and +30◦, contains several giant star forming molecular cloud complexes located at various distances from arXiv:0809.4761v1 [astro-ph] 27 Sep 2008 the Sun.
    [Show full text]