TIME 1. Introduction 2. Time Scales
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Daylight Saving Time
Daylight Saving Time Beth Cook Information Research Specialist March 9, 2016 Congressional Research Service 7-5700 www.crs.gov R44411 Daylight Saving Time Summary Daylight Saving Time (DST) is a period of the year between spring and fall when clocks in the United States are set one hour ahead of standard time. DST is currently observed in the United States from 2:00 a.m. on the second Sunday in March until 2:00 a.m. on the first Sunday in November. The following states and territories do not observe DST: Arizona (except the Navajo Nation, which does observe DST), Hawaii, American Samoa, Guam, the Northern Mariana Islands, Puerto Rico, and the Virgin Islands. Congressional Research Service Daylight Saving Time Contents When and Why Was Daylight Saving Time Enacted? .................................................................... 1 Has the Law Been Amended Since Inception? ................................................................................ 2 Which States and Territories Do Bot Observe DST? ...................................................................... 2 What Other Countries Observe DST? ............................................................................................. 2 Which Federal Agency Regulates DST in the United States? ......................................................... 3 How Does an Area Move on or off DST? ....................................................................................... 3 How Can States and Territories Change an Area’s Time Zone? ..................................................... -
Ast 443 / Phy 517
AST 443 / PHY 517 Astronomical Observing Techniques Prof. F.M. Walter I. The Basics The 3 basic measurements: • WHERE something is • WHEN something happened • HOW BRIGHT something is Since this is science, let’s be quantitative! Where • Positions: – 2-dimensional projections on celestial sphere (q,f) • q,f are angular measures: radians, or degrees, minutes, arcsec – 3-dimensional position in space (x,y,z) or (q, f, r). • (x,y,z) are linear positions within a right-handed rectilinear coordinate system. • R is a distance (spherical coordinates) • Galactic positions are sometimes presented in cylindrical coordinates, of galactocentric radius, height above the galactic plane, and azimuth. Angles There are • 360 degrees (o) in a circle • 60 minutes of arc (‘) in a degree (arcmin) • 60 seconds of arc (“) in an arcmin There are • 24 hours (h) along the equator • 60 minutes of time (m) per hour • 60 seconds of time (s) per minute • 1 second of time = 15”/cos(latitude) Coordinate Systems "What good are Mercator's North Poles and Equators Tropics, Zones, and Meridian Lines?" So the Bellman would cry, and the crew would reply "They are merely conventional signs" L. Carroll -- The Hunting of the Snark • Equatorial (celestial): based on terrestrial longitude & latitude • Ecliptic: based on the Earth’s orbit • Altitude-Azimuth (alt-az): local • Galactic: based on MilKy Way • Supergalactic: based on supergalactic plane Reference points Celestial coordinates (Right Ascension α, Declination δ) • δ = 0: projection oF terrestrial equator • (α, δ) = (0,0): -
Ephemeris Time, D. H. Sadler, Occasional
EPHEMERIS TIME D. H. Sadler 1. Introduction. – At the eighth General Assembly of the International Astronomical Union, held in Rome in 1952 September, the following resolution was adopted: “It is recommended that, in all cases where the mean solar second is unsatisfactory as a unit of time by reason of its variability, the unit adopted should be the sidereal year at 1900.0; that the time reckoned in these units be designated “Ephemeris Time”; that the change of mean solar time to ephemeris time be accomplished by the following correction: ΔT = +24°.349 + 72s.318T + 29s.950T2 +1.82144 · B where T is reckoned in Julian centuries from 1900 January 0 Greenwich Mean Noon and B has the meaning given by Spencer Jones in Monthly Notices R.A.S., Vol. 99, 541, 1939; and that the above formula define also the second. No change is contemplated or recommended in the measure of Universal Time, nor in its definition.” The ultimate purpose of this article is to explain, in simple terms, the effect that the adoption of this resolution will have on spherical and dynamical astronomy and, in particular, on the ephemerides in the Nautical Almanac. It should be noted that, in accordance with another I.A.U. resolution, Ephemeris Time (E.T.) will not be introduced into the national ephemerides until 1960. Universal Time (U.T.), previously termed Greenwich Mean Time (G.M.T.), depends both on the rotation of the Earth on its axis and on the revolution of the Earth in its orbit round the Sun. There is now no doubt as to the variability, both short-term and long-term, of the rate of rotation of the Earth; U.T. -
An Introduction to Orbit Dynamics and Its Application to Satellite-Based Earth Monitoring Systems
19780004170 NASA-RP- 1009 78N12113 An introduction to orbit dynamics and its application to satellite-based earth monitoring systems NASA Reference Publication 1009 An Introduction to Orbit Dynamics and Its Application to Satellite-Based Earth Monitoring Missions David R. Brooks Langley Research Center Hampton, Virginia National Aeronautics and Space Administration Scientific and Technical Informalion Office 1977 PREFACE This report provides, by analysis and example, an appreciation of the long- term behavior of orbiting satellites at a level of complexity suitable for the initial phases of planning Earth monitoring missions. The basic orbit dynamics of satellite motion are covered in detail. Of particular interest are orbit plane precession, Sun-synchronous orbits, and establishment of conditions for repetitive surface coverage. Orbit plane precession relative to the Sun is shown to be the driving factor in observed patterns of surface illumination, on which are superimposed effects of the seasonal motion of the Sun relative to the equator. Considerable attention is given to the special geometry of Sun- synchronous orbits, orbits whose precession rate matches the average apparent precession rate of the Sun. The solar and orbital plane motions take place within an inertial framework, and these motions are related to the longitude- latitude coordinates of the satellite ground track through appropriate spatial and temporal coordinate systems. It is shown how orbit parameters can be chosen to give repetitive coverage of the same set of longitude-latitude values on a daily or longer basis. Several potential Earth monitoring missions which illus- trate representative applications of the orbit dynamics are described. The interactions between orbital properties and the resulting coverage and illumina- tion patterns over specific sites on the Earth's surface are shown to be at the heart of satellite mission planning. -
Daylight Saving Time (DST)
Daylight Saving Time (DST) Updated September 30, 2020 Congressional Research Service https://crsreports.congress.gov R45208 Daylight Saving Time (DST) Summary Daylight Saving Time (DST) is a period of the year between spring and fall when clocks in most parts of the United States are set one hour ahead of standard time. DST begins on the second Sunday in March and ends on the first Sunday in November. The beginning and ending dates are set in statute. Congressional interest in the potential benefits and costs of DST has resulted in changes to DST observance since it was first adopted in the United States in 1918. The United States established standard time zones and DST through the Calder Act, also known as the Standard Time Act of 1918. The issue of consistency in time observance was further clarified by the Uniform Time Act of 1966. These laws as amended allow a state to exempt itself—or parts of the state that lie within a different time zone—from DST observance. These laws as amended also authorize the Department of Transportation (DOT) to regulate standard time zone boundaries and DST. The time period for DST was changed most recently in the Energy Policy Act of 2005 (EPACT 2005; P.L. 109-58). Congress has required several agencies to study the effects of changes in DST observance. In 1974, DOT reported that the potential benefits to energy conservation, traffic safety, and reductions in violent crime were minimal. In 2008, the Department of Energy assessed the effects to national energy consumption of extending DST as changed in EPACT 2005 and found a reduction in total primary energy consumption of 0.02%. -
An Atomic Physics Perspective on the New Kilogram Defined by Planck's Constant
An atomic physics perspective on the new kilogram defined by Planck’s constant (Wolfgang Ketterle and Alan O. Jamison, MIT) (Manuscript submitted to Physics Today) On May 20, the kilogram will no longer be defined by the artefact in Paris, but through the definition1 of Planck’s constant h=6.626 070 15*10-34 kg m2/s. This is the result of advances in metrology: The best two measurements of h, the Watt balance and the silicon spheres, have now reached an accuracy similar to the mass drift of the ur-kilogram in Paris over 130 years. At this point, the General Conference on Weights and Measures decided to use the precisely measured numerical value of h as the definition of h, which then defines the unit of the kilogram. But how can we now explain in simple terms what exactly one kilogram is? How do fixed numerical values of h, the speed of light c and the Cs hyperfine frequency νCs define the kilogram? In this article we give a simple conceptual picture of the new kilogram and relate it to the practical realizations of the kilogram. A similar change occurred in 1983 for the definition of the meter when the speed of light was defined to be 299 792 458 m/s. Since the second was the time required for 9 192 631 770 oscillations of hyperfine radiation from a cesium atom, defining the speed of light defined the meter as the distance travelled by light in 1/9192631770 of a second, or equivalently, as 9192631770/299792458 times the wavelength of the cesium hyperfine radiation. -
Building the Bridge Between the First and Second Year Experience: a Collaborative Approach to Student Learning and Development STEP
Building the bridge between the first and second year experience: A collaborative approach to student learning and development STEP Introductions STEP Agenda for Today • Share research and theory that shapes first and second year programs • Differentiate programs, interventions, and support that should be targeted at first year students, second year students, or both • Think about your own department and how to work differently with first and second-year students • Review structure of FYE and STEP at Ohio State and where your office can support existing efforts STEP Learning Outcomes • Participants will reflect on and articulate what services, resources, and programming currently exist in their department for first and/or second year students. • Participants will articulate the key salient needs and developmental milestones that often distinguish the second year experience from the first. • Participants will be able to utilize at least one strategy for curriculum differentiation that will contribute to a more seamless experiences for students between their first and second year. Foundational Research that Informs FYE and STEP STEP Developmental Readiness and Sequencing • Developmental Readiness: “The ability and motivation to attend to, make meaning of, and appropriate new knowledge into one’s long term memory structures” (Hannah & Lester, 2009). • Sequencing: The order and structure in which people learn new skill sets (Hannah & Avolio, 2010). • Scaffolding: Support given during the learning process which is tailored to the needs of an -
Second Time Moms & the Truth About Parenting
Second Time Moms & The Truth About Parenting Summary Why does our case deserve an award? In the US, and globally, every diaper brand obsesses about the emotion and joy experienced by new parents. Luvs took the brave decision to focus exclusively on an audience that nobody was talking to: second time moms. Planning made Luvs the official diaper brand of experienced moms. The depth of insights Planning uncovered about this target led to creative work that did a very rare thing for the diaper category: it was funny, entertaining and sparked a record amount of debate. For the first time these moms felt that someone was finally standing up for them and Luvs was applauded for not being afraid to show motherhood in a more realistic way. And in doing so, we achieved the highest volume and value sales in the brand’s history. 2 Luvs: A Challenger Facing A Challenge Luvs is a value priced diaper brand that ranks a distant fourth in terms of value share within the US diaper category at 8.9%. Pampers and Huggies are both premium priced diapers that make up most of the category, with value share at 31, and 41 respectively. Private Label is the third biggest player with 19% value share. We needed to generate awareness to drive trial for Luvs in order to grow the brand, but a few things stood in our way. Low Share Of Voice Huggies spends $54 million on advertising and Pampers spends $48 million. In comparison, Luvs spends only $9 million in media support. So the two dominant diaper brands outspend us 9 to 1, making our goal of increased awareness very challenging. -
HOW FAST IS RF? by RON HRANAC
Originally appeared in the September 2008 issue of Communications Technology. HOW FAST IS RF? By RON HRANAC Maybe a better question is, "What's the speed of an electromagnetic signal in a vacuum?" After all, what we call RF refers to signals in the lower frequency or longer wavelength part of the electromagnetic spectrum. Light is an electromagnetic signal, too, existing in the higher frequency or shorter wavelength part of the electromagnetic spectrum. One way to look at it is to assume that RF is nothing more than really, really low frequency light, or that light is really, really high frequency RF. As you might imagine, the numbers involved in describing RF and light can be very large or very small. For more on this, see my June 2007 CT column, "Big Numbers, Small Numbers" (www.cable360.net/ct/operations/techtalk/23783.html). According to the National Institute of Standards and Technology, the speed of light in a vacuum, c0, is 299,792,458 meters per second (http://physics.nist.gov/cgi-bin/cuu/Value?c). The designation c0 is one that NIST uses to reference the speed of light in a vacuum, while c is occasionally used to reference the speed of light in some other medium. Most of the time the subscript zero is dropped, with c being a generic designation for the speed of light. Let's put c0 in terms that may be more familiar. You probably recall from junior high or high school science class that the speed of light is 186,000 miles per second. -
How Long Is a Year.Pdf
How Long Is A Year? Dr. Bryan Mendez Space Sciences Laboratory UC Berkeley Keeping Time The basic unit of time is a Day. Different starting points: • Sunrise, • Noon, • Sunset, • Midnight tied to the Sun’s motion. Universal Time uses midnight as the starting point of a day. Length: sunrise to sunrise, sunset to sunset? Day Noon to noon – The seasonal motion of the Sun changes its rise and set times, so sunrise to sunrise would be a variable measure. Noon to noon is far more constant. Noon: time of the Sun’s transit of the meridian Stellarium View and measure a day Day Aday is caused by Earth’s motion: spinning on an axis and orbiting around the Sun. Earth’s spin is very regular (daily variations on the order of a few milliseconds, due to internal rearrangement of Earth’s mass and external gravitational forces primarily from the Moon and Sun). Synodic Day Noon to noon = synodic or solar day (point 1 to 3). This is not the time for one complete spin of Earth (1 to 2). Because Earth also orbits at the same time as it is spinning, it takes a little extra time for the Sun to come back to noon after one complete spin. Because the orbit is elliptical, when Earth is closest to the Sun it is moving faster, and it takes longer to bring the Sun back around to noon. When Earth is farther it moves slower and it takes less time to rotate the Sun back to noon. Mean Solar Day is an average of the amount time it takes to go from noon to noon throughout an orbit = 24 Hours Real solar day varies by up to 30 seconds depending on the time of year. -
The Determination of Longitude in Landsurveying.” by ROBERTHENRY BURNSIDE DOWSES, Assoc
316 DOWNES ON LONGITUDE IN LAXD SUIWETISG. [Selected (Paper No. 3027.) The Determination of Longitude in LandSurveying.” By ROBERTHENRY BURNSIDE DOWSES, Assoc. M. Inst. C.E. THISPaper is presented as a sequel tothe Author’s former communication on “Practical Astronomy as applied inLand Surveying.”’ It is not generally possible for a surveyor in the field to obtain accurate determinationsof longitude unless furnished with more powerful instruments than is usually the case, except in geodetic camps; still, by the methods here given, he may with care obtain results near the truth, the error being only instrumental. There are threesuch methods for obtaining longitudes. Method 1. By Telrgrcrph or by Chronometer.-In either case it is necessary to obtain the truemean time of the place with accuracy, by means of an observation of the sun or z star; then, if fitted with a field telegraph connected with some knownlongitude, the true mean time of that place is obtained by telegraph and carefully compared withthe observed true mean time atthe observer’s place, andthe difference between thesetimes is the difference of longitude required. With a reliable chronometer set totrue Greenwich mean time, or that of anyother known observatory, the difference between the times of the place and the time of the chronometer must be noted, when the difference of longitude is directly deduced. Thisis the simplest method where a camp is furnisl~ed with eitherof these appliances, which is comparatively rarely the case. Method 2. By Lunar Distances.-This observation is one requiring great care, accurately adjusted instruments, and some littleskill to obtain good results;and the calculations are somewhat laborious. -
Low Latency – How Low Can You Go?
WHITE PAPER Low Latency – How Low Can You Go? Low latency has always been an important consideration in telecom networks for voice, video, and data, but recent changes in applications within many industry sectors have brought low latency right to the forefront of the industry. The finance industry and algorithmic trading in particular, or algo-trading as it is known, is a commonly quoted example. Here latency is critical, and to quote Information Week magazine, “A 1-millisecond advantage in trading applications can be worth $100 million a year to a major brokerage firm.” This drives a huge focus on all aspects of latency, including the communications systems between the brokerage firm and the exchange. However, while the finance industry is spending a lot of money on low- latency services between key locations such as New York and Chicago or London and Frankfurt, this is actually only a small part of the wider telecom industry. Many other industries are also now driving lower and lower latency in their networks, such as for cloud computing and video services. Also, as mobile operators start to roll out 5G services, latency in the xHaul mobile transport network, especially the demanding fronthaul domain, becomes more and more important in order to reach the stringent 5G requirements required for the new class of ultra-reliable low-latency services. This white paper will address the drivers behind the recent rush to low- latency solutions and networks and will consider how network operators can remove as much latency as possible from their networks as they also race to zero latency.