A Recommendation - Amateur Astronomers, Inc.
... (the region just beyond the orbit of Neptune that is home to icy objects such as Makemake, Eris, and Pluto as well as a large number of potential comets), but rather from the Oort Cloud, a region of space that extends beyond the Kuiper Belt out to about one light year from the Sun. Based on the orbi ...
... (the region just beyond the orbit of Neptune that is home to icy objects such as Makemake, Eris, and Pluto as well as a large number of potential comets), but rather from the Oort Cloud, a region of space that extends beyond the Kuiper Belt out to about one light year from the Sun. Based on the orbi ...
Marking Scheme of Observational Sessions
... observer can mark those Deep Sky Objects ( IF THEY CAN BE SEEN IN NAKED EYE ) by using standard symbols . Eg : - Observer can mark Orion nebula (by a Symbol) in its position ( at the constellation of “Orion”) in his/her constellation mapping drawing. But drawing Orion nebula IS NOT ACCEPTABLE ! Maxi ...
... observer can mark those Deep Sky Objects ( IF THEY CAN BE SEEN IN NAKED EYE ) by using standard symbols . Eg : - Observer can mark Orion nebula (by a Symbol) in its position ( at the constellation of “Orion”) in his/her constellation mapping drawing. But drawing Orion nebula IS NOT ACCEPTABLE ! Maxi ...
Constraining the star formation histories of spiral bulges
... Stellar populations in spiral bulges are investigated using the Lick system of spectral indices. Long-slit spectroscopic observations of line strengths and kinematics made along the minor axes of four spiral bulges are reported. Comparisons are made between central line strengths in spiral bulges an ...
... Stellar populations in spiral bulges are investigated using the Lick system of spectral indices. Long-slit spectroscopic observations of line strengths and kinematics made along the minor axes of four spiral bulges are reported. Comparisons are made between central line strengths in spiral bulges an ...
Sparse aperture masking at the VLT II. Detection limits for the eight
... of the χ2 maps allows for the extraction of detection limits. Detection limit maps from the SAM pipeline are expressed in contrast ratio. Hence, the L0 band detection limits depend on the brightness of the parent star. We used the spectral type of the stars (given in Table 2), combined with Tokunaga ...
... of the χ2 maps allows for the extraction of detection limits. Detection limit maps from the SAM pipeline are expressed in contrast ratio. Hence, the L0 band detection limits depend on the brightness of the parent star. We used the spectral type of the stars (given in Table 2), combined with Tokunaga ...
neutron star
... galaxies are richer in heavy elements than the Sun, with the highest abundances ever seen in the early Universe. Heavy elements that enrich mature galaxies in the local Universe were made in past generations of stars. So these young galaxies have experienced a prodigious rate of star formation and c ...
... galaxies are richer in heavy elements than the Sun, with the highest abundances ever seen in the early Universe. Heavy elements that enrich mature galaxies in the local Universe were made in past generations of stars. So these young galaxies have experienced a prodigious rate of star formation and c ...
... 2419130.305+0.28779276 E is reproduced in Figure 4. Visual observations show a particularly large scatter at HJD ∼ 2443800 which may be due to their larger uncertainty. We have included them for completeness, but if they are ignored the O-C diagram strongly suggests an abrupt period change some time ...
PDF - ASSA
... units apart, and given that they are each around nine solar masses the orbital period must be at least 20 000 years. But there is more! Located just 5' south-east is the fainter, wider, more-equal pair HJ 4252, which shares the field with upsilon in a 150-mm f/8 refractor at 136x. This second set con ...
... units apart, and given that they are each around nine solar masses the orbital period must be at least 20 000 years. But there is more! Located just 5' south-east is the fainter, wider, more-equal pair HJ 4252, which shares the field with upsilon in a 150-mm f/8 refractor at 136x. This second set con ...
A Star - Cloudy Nights
... bluish tint. The pair are about 410 light years distant and are separated by 4400 A.U. Mizar is a fine example of a double star system. This pair lies at a distance of 88 light years and are separated by 380 A.U. Observations indicate that it must take several thousand years for these two stars to ...
... bluish tint. The pair are about 410 light years distant and are separated by 4400 A.U. Mizar is a fine example of a double star system. This pair lies at a distance of 88 light years and are separated by 380 A.U. Observations indicate that it must take several thousand years for these two stars to ...
hwd_ewd_v3 - X-ray and Observational Astronomy Group
... INTRODUCTION Theoretical and observational study of stellar behaviour has provided white dwarfs with their evolutionary context as one end point of the life-cycle of stars. In general terms, all stars with masses below about eight times that of the Sun will pass through one or more red giant phases ...
... INTRODUCTION Theoretical and observational study of stellar behaviour has provided white dwarfs with their evolutionary context as one end point of the life-cycle of stars. In general terms, all stars with masses below about eight times that of the Sun will pass through one or more red giant phases ...
Rocky planetesimals as the origin of metals in DZ stars
... where hydrogen is detected or inferred (Dufour et al. 2007) versus height above the Galactic mid-plane and tangential speed. No obvious pattern is seen, although there may be a higher density of DZA stars near the Galactic disc and perhaps also towards more modest speeds, but the former may be an ob ...
... where hydrogen is detected or inferred (Dufour et al. 2007) versus height above the Galactic mid-plane and tangential speed. No obvious pattern is seen, although there may be a higher density of DZA stars near the Galactic disc and perhaps also towards more modest speeds, but the former may be an ob ...
Properties of Wolf-Rayet Stars - Paul Crowther, University of Sheffield
... ratios (Smith 1968). To date, high-ionization WN2 to WN5 are known as ‘early WN’ (WNE) stars, and low-ionization WN7 to WN9(–11) stars known as ‘late WN’ (WNL) stars, and WN6 stars either early or late-type. Complications arise for WN stars with intrinsically weak emission lines. For example, HD 931 ...
... ratios (Smith 1968). To date, high-ionization WN2 to WN5 are known as ‘early WN’ (WNE) stars, and low-ionization WN7 to WN9(–11) stars known as ‘late WN’ (WNL) stars, and WN6 stars either early or late-type. Complications arise for WN stars with intrinsically weak emission lines. For example, HD 931 ...
The Extragalactic Group of MPE and USM
... of Massive Galaxies in the FORS Deep and GOODS South fields • Study evolution of galaxies with broadband deep U to K surveys. • LFs, Mass Functions, SFRs do not require spectroscopy but can be derived with accurate photometric redshifts. • Advantage of photo z: no color selection bias, fainter lumin ...
... of Massive Galaxies in the FORS Deep and GOODS South fields • Study evolution of galaxies with broadband deep U to K surveys. • LFs, Mass Functions, SFRs do not require spectroscopy but can be derived with accurate photometric redshifts. • Advantage of photo z: no color selection bias, fainter lumin ...
3-1
... B. 0.6 + 0.008 + 0.0007 Standard form: 0.6087 Word form: six thousand eighty-seven tenthousandths Course 1 ...
... B. 0.6 + 0.008 + 0.0007 Standard form: 0.6087 Word form: six thousand eighty-seven tenthousandths Course 1 ...
A Digital Spectral Classification Atlas
... MK system is defined by a set of standard stars, and classification on the system is carried out by the comparison of the program star with the standard stars, taking into account all of the features in the spectrum. The use of standards is vital because it maintains the autonomy of the system as we ...
... MK system is defined by a set of standard stars, and classification on the system is carried out by the comparison of the program star with the standard stars, taking into account all of the features in the spectrum. The use of standards is vital because it maintains the autonomy of the system as we ...
CHAPTER 1 The Formation and Structure of Stars
... • How do astronomers know there is an interstellar medium, and how do they know its properties? – In some cases, the interstellar medium is easily visible as clouds of gas and dust—as in the case of the Great Nebula in Orion. – Astronomers call such a cloud a nebula—from the Latin word for cloud. – ...
... • How do astronomers know there is an interstellar medium, and how do they know its properties? – In some cases, the interstellar medium is easily visible as clouds of gas and dust—as in the case of the Great Nebula in Orion. – Astronomers call such a cloud a nebula—from the Latin word for cloud. – ...
Life Histories Of Some Stars
... graph? Where do newborn babies cluster? Children? Or is there no clustering at all? Describe the shape of the graph? Is it a straight line? A curve? 5. Give each group the list of stars attached and the HR diagram attached. Instead of height and weight, the information is in Luminosity (compared to ...
... graph? Where do newborn babies cluster? Children? Or is there no clustering at all? Describe the shape of the graph? Is it a straight line? A curve? 5. Give each group the list of stars attached and the HR diagram attached. Instead of height and weight, the information is in Luminosity (compared to ...
Star formation in a galactic outflow
... population with kinematical fingerprints of formation inside the outflow. The stellar continuum is detected in the X-shooter spectra out to about 5 kpc from the nucleus, and its shape and stellar features do indeed indicate the presence of a young stellar population younger than a few tens of millio ...
... population with kinematical fingerprints of formation inside the outflow. The stellar continuum is detected in the X-shooter spectra out to about 5 kpc from the nucleus, and its shape and stellar features do indeed indicate the presence of a young stellar population younger than a few tens of millio ...
A spectroscopic investigation of the O
... Methods. We performed a long-term spectroscopic survey of nineteen O-type stars. We searched for radial velocity variations to unveil binaries on timescales from a few days up to a few years, on the basis of a large set of optical spectra. Results. We confirm the binarity for four objects: HD 193443 ...
... Methods. We performed a long-term spectroscopic survey of nineteen O-type stars. We searched for radial velocity variations to unveil binaries on timescales from a few days up to a few years, on the basis of a large set of optical spectra. Results. We confirm the binarity for four objects: HD 193443 ...
The first carbon-enhanced metal-poor star found in the Sculptor
... The origin of carbon-enhanced metal-poor (CEMP) stars and their possible connection with the chemical elements produced by the first stellar generation is still highly debated. In contrast to the Galactic halo, not many CEMP stars have been found in the dwarf spheroidal galaxies around the Milky Way ...
... The origin of carbon-enhanced metal-poor (CEMP) stars and their possible connection with the chemical elements produced by the first stellar generation is still highly debated. In contrast to the Galactic halo, not many CEMP stars have been found in the dwarf spheroidal galaxies around the Milky Way ...
How to Build an Astrolabe
... the brightest stars in the sky. Its name is derived from Arabic, and means "the follower", as it appears to follow the cluster of stars known as The Pleiades across the sky. Altair (α Aquilae): the brightest star in the constellation of Aquila, the Eagle. Arcturus (α Boötis): part of the constellati ...
... the brightest stars in the sky. Its name is derived from Arabic, and means "the follower", as it appears to follow the cluster of stars known as The Pleiades across the sky. Altair (α Aquilae): the brightest star in the constellation of Aquila, the Eagle. Arcturus (α Boötis): part of the constellati ...
Boötes
Boötes /boʊˈoʊtiːz/ is a constellation in the northern sky, located between 0° and +60° declination, and 13 and 16 hours of right ascension on the celestial sphere. The name comes from the Greek Βοώτης, Boōtēs, meaning herdsman or plowman (literally, ox-driver; from βοῦς bous “cow”). The ""ö"" in the name is a diaeresis, not an umlaut, meaning that each 'o' is to be pronounced separately.One of the 48 constellations described by the 2nd century astronomer Ptolemy, Boötes is now one of the 88 modern constellations. It contains the fourth brightest star in the night sky, the orange-hued Arcturus. Boötes is home to many other bright stars, including eight above the fourth magnitude and an additional 21 above the fifth magnitude, making a total of 29 stars easily visible to the naked eye.