Last edited by Kilkis
Saturday, July 18, 2020 | History

2 edition of mass of AW Ursae Majoris found in the catalog.

mass of AW Ursae Majoris

Michael J. Rensing

mass of AW Ursae Majoris

by Michael J. Rensing

  • 145 Want to read
  • 0 Currently reading

Published by University of Toronto in Toronto .
Written in English


Edition Notes

Thesis (M.Sc.)--University of Toronto, 1984.

Statementby Michael J. Rensing.
ID Numbers
Open LibraryOL14856229M

Megrez, Delta Ursae Majoris (δ UMa), is the faintest of the seven stars that form the Big Dipper asterism. It is a third magnitude star with an apparent magnitude . Alioth (Epsilon Ursae Majoris), despite its “epsilon” tag, is the most luminous star in Ursa Major but only just since at magnitude + it is a mere 2% brighter than the star Dubhe, the second brightest star in the ed light years from Earth, this blue star is also the 33rd brightest star in the entire night sky, and is listed as one of the 57 navigational stars.

Eta Ursae Majoris (Latinised from η Ursae Majoris, abbreviated Eta UMa, η UMa), formally named Alkaid / æ l ˈ k eɪ d /, is a star in the constellation of Ursa is the most eastern (leftmost) star in the Big Dipper (or Plough) r, unlike most stars of the Big Dipper, it is not a member of the Ursa Major moving group. With an apparent visual magnitude of +, it is. The discovery of 47 Ursae Majoris b was announced in Orbit and mass Edit 47 Ursae Majoris b orbits at a distance of AU from its star, taking 1, days or years to complete a revolution. It was the first long .

DK Cyg (P = ) is a W Ursae Majoris type eclipsing binary system that undergoes complete eclipses. All the published photoelectric data have been collected and utilized to re-examine and. Phecda (Gamma Ursae Majoris), the 6th brightest star in Ursa Major and 85th brightest star in the night sky, marks out the lower left corner of the Big Dipper’s bowl. Along with most of the Dipper’s stars, Phecda is an inner member of the Ursa Major Moving Group, which is a relatively large group of stars (which may include Sirius) that.


Share this book
You might also like
What is direct access?

What is direct access?

Sequential nitrification/denitrification in subsurface flow constructed wetlands

Sequential nitrification/denitrification in subsurface flow constructed wetlands

Chapman Piloting Seamanship and Small Boat Handling

Chapman Piloting Seamanship and Small Boat Handling

Directory of firms registered

Directory of firms registered

Grass roots self reliance in Shramik Sanghatana, Dhulia district, India

Grass roots self reliance in Shramik Sanghatana, Dhulia district, India

Yours faithfully, Yogi

Yours faithfully, Yogi

Convergence of recursive learning mechanisms to steady states and cycles in stochastic nonlinear models

Convergence of recursive learning mechanisms to steady states and cycles in stochastic nonlinear models

The coin collectors fact book

The coin collectors fact book

Esther A. George.

Esther A. George.

Optimisation and Stability Theory for Economic Analysis

Optimisation and Stability Theory for Economic Analysis

No 4-Legged Meat Please

No 4-Legged Meat Please

The 2000 Import and Export Market for Textile and Leather Machinery and Equipment in Albania

The 2000 Import and Export Market for Textile and Leather Machinery and Equipment in Albania

Toward a film humanism

Toward a film humanism

Facts about the E.E.C.

Facts about the E.E.C.

Mass of AW Ursae Majoris by Michael J. Rensing Download PDF EPUB FB2

The mass of AW Ursae Majoris was found to be + or - solar masses, if the mass ratio q isand + or - solar masses if q = Such masses are much smaller than the values.

AW Ursae Majoris estimated radius has been calculated as being times bigger than the Sun. The Sun's radius is ,km, therefore the star's radius is an estimated 1,km. If you need the diameter of the star, you just need to multiple the radius by 2. The mass of AW Ursae Majoris was found to be + or - solar masses, if the mass ratio q isand + or - solar masses if q = Such masses are much smaller than the values found in previous studies.

The new result agrees well with evolutionary theories of contact binaries if A W UMa is a terminal-age main-sequence by:   Joel A. Eaton, AW Ursae Majoris: a semidetached mass-transferring system indeed?, Monthly Notices of the Royal Astronomical Society, VolumeIssue 1, 21 MarchPages –, for the hot A-type W Ursae Majoris binary AW UMa in terms of various contact models, finding that the detached/semidetached geometry he postulates does not Cited by: 2.

I have reinterpreted Rucinski's line profiles (broadening functions) for the hot A-type W Ursae Majoris binary AW UMa in terms of various contact models, finding that the detached/semidetached geometry he postulates does not fit the system's light variation or its line profiles.

The highly overcontact geometry that actually fits the system's ellipsoidal light variation reproduce the total Cited by: 2. As a result, the components share a common envelope.

Li et al. () found that most W UMa systems might be formed from detached binaries with periods less than/approximately days and a maximum advanced time from a detached system to a W UMa to be about Gyr.

Two Groups Proposed. 16 rows  From Wikipedia, the free encyclopedia Schematic of a W Ursae Majoris variable with a. W Ursae Majoris (W UMa) is the variable star designation for a binary star system in the northern constellation of Ursa Major.

It has an apparent visual magnitude of aboutwhich is too faint to be seen with the naked eye. However, it can be viewed with a small telescope. α Ursae Majoris, known by the Arabic name Dubhe ("the bear"), which at a magnitude of is the 35th-brightest star in the sky and the second-brightest of Ursa Major.; β Ursae Majoris, called Merak ("the loins of the bear"), with a magnitude of ; γ Ursae Majoris, known as either Phecda or Phad ("thigh"), with a magnitude of ; δ Ursae Majoris, or Megrez, meaning "root of the.

Iota Ursae Majoris (ι Ursae Majoris, abbreviated Iota UMa, ι UMa), also named Talitha / ˈ t æ l ɪ θ ə /, is a star system in the northern circumpolar constellation of Ursa has an apparent visual magnitude ofmaking it visible to the naked eye and placing it among the brighter members of this constellation.

Based upon parallax measurements, it is located at a distance of. The minimum mass ratio for tidal stability of a contact binary containing two unevolved main-sequence stars is calculated to be $\qmin\simeq$ in the case of a mostly radiative primary, and is higher if an appreciable fraction of the mass lies in a convective envelope.

W Ursae Majoris: Mass-Ratio Discrepancy, Third Body and Age Article (PDF Available) in Monthly Notices of the Royal Astronomical Society (1). A method for the syntbesis of theoretical ligbt curves and line profiles for close binary systems is outlined, considering Roche geometry, non-linear limb-darkening and convective envelopes with irradiation and gravitydarkening.

A scaled blackbody approximation is used for calculating fluxes. Theoretical internal eclipse contact angles have been computed for common envelope configurations.

@article{osti_, title = {TIME-VARIABLE ALUMINUM ABSORPTION IN THE POLAR AR URSAE MAJORIS, AND AN UPDATED ESTIMATE FOR THE MASS OF THE WHITE DWARF}, author = {Bai, Yu and Justham, Stephen and Liu, JiFeng and Guo, JinCheng and Gao, Qing and Gong, Hang}, abstractNote = {We present spectra of the extreme polar AR Ursae Majoris (AR UMa), which display.

– Phecda (Gamma Ursae Majoris) is a white main sequence star 84 light-years distant that shines with a magnitude of It is about 71 times brighter than the Sun.

– Megrez (Delta Ursae Majoris) is a blue-white star light years from Earth with a magnitude of It is 63% more massive than our sun, and is 14 times more luminous.

47 Ursae Majoris (abbreviated 47 UMa) is a yellow dwarf star similar to our Sun located approximately 46 light-years away in the constellation Ursa Major. As of47 Ursae Majoris is known to have two extrasolar planets orbiting it. 47 Ursae Majoris is ranked 72nd in the list of top target stars for the NASA Terrestrial Planet Finder mission.

A solar analog, with a spectral type of G1V, it has a similar mass to that of the Sun but is slightly hotter at around 5, K. and slightly more metal-rich with around % of the solar abundance of iron.

Like the Sun, 47 Ursae Majoris is on the main sequence, converting hydrogen to. Mizar / ˈ m aɪ z ɑːr / is a second-magnitude star in the handle of the Big Dipper asterism in the constellation of Ursa has the Bayer designation ζ Ursae Majoris (Latinised as Zeta Ursae Majoris).It forms a well-known naked eye double star with the fainter star Alcor, and is itself a quadruple star whole system lies about 83 light-years away from the Sun, as measured.

New and published UBV photoelectric and spectroscopic observations of AW UMa are analyzed and interpreted by a triple or quadruple-star model. The derived inclination angle i = °, the photometric mass ratio q = as well as all available radial velocities, corrected for the systemic velocity changes, were used to determine the masses of the components of the contact binary as M_1 = (1.

There is also second spectroscopic companion located 8 minutes of arc away from the primary star, which is a 7th magnitude F8-type star listed as Alpha Ursae Majoris C (HD ). In addition to the primary pair, another binary system is located ab astronomical units away, which makes Dubhe a 5-star system.

Alkaid (Eta Ursae Majoris) is a prominent star in the handle of the Big Dipper, an asterism which forms just a small part of the overall constellation of Ursa Major. With an apparent magnitude of +, it is the third most luminous star in Ursa Major, and the 38th most luminous star in the entire night sky.The dust has an estimated mass of about % the mass of the Earth.

Beta Ursae Majoris is one of five stars in the Big Dipper that form a part of a loose open cluster called the Ursa Major moving group, sharing the same region of space and not just the same patch of sky from Earth's perspective. This group has an estimated age of about 47 Ursae Majoris b is an extrasolar planet orbiting the Sun-like star 47 Ursae is located in a long-period, near-circular orbit and is the innermost known planet in its planetary system.

47 Ursae Majoris b was discovered in and has a mass at least times that of ery. Like the majority of known extrasolar planets, 47 Ursae Majoris b was discovered by detecting.