Constraints on Long-Period Planets from an L
... would be fascinating, we also need information about systems old enough to have settled down into a mature, stable configuration. To probe long-period planet populations in mature systems, surveys such as ours that target older stars are necessary. Additionally, theoretical spectra of older planets ...
... would be fascinating, we also need information about systems old enough to have settled down into a mature, stable configuration. To probe long-period planet populations in mature systems, surveys such as ours that target older stars are necessary. Additionally, theoretical spectra of older planets ...
Abstracts - Physics of Evolved Stars 2015
... intermediate main-sequence mass (5-8 solar masses) stars before they evolve into the post-AGB and planetary-nebula stages. AGB stars lose most of their stellar envelope in the form of a gaseous and dusty stellar wind. This wind eventually grows to such high mass-loss rates that the central star beco ...
... intermediate main-sequence mass (5-8 solar masses) stars before they evolve into the post-AGB and planetary-nebula stages. AGB stars lose most of their stellar envelope in the form of a gaseous and dusty stellar wind. This wind eventually grows to such high mass-loss rates that the central star beco ...
The local spiral structure of the Milky Way
... Perseus. Toward the constellation Cygnus, sources in the Local Arm extend for a great distance along our line of sight and roughly along the solar orbit. Because of this orientation, these sources cluster both on the sky and in velocity to form the complex and long enigmatic Cygnus X region. We also ...
... Perseus. Toward the constellation Cygnus, sources in the Local Arm extend for a great distance along our line of sight and roughly along the solar orbit. Because of this orientation, these sources cluster both on the sky and in velocity to form the complex and long enigmatic Cygnus X region. We also ...
The DBV stars: Progress and problems
... would need 2.5m telescopes to get the same signal-to-noise temporal spectroscopy, assuming everything else is equal. This presents a real problem for the WET in resolving the modal structure of the other DBV stars, and we are at a crossroads with the 1995 May run,with PG 13513-489 as the primary tar ...
... would need 2.5m telescopes to get the same signal-to-noise temporal spectroscopy, assuming everything else is equal. This presents a real problem for the WET in resolving the modal structure of the other DBV stars, and we are at a crossroads with the 1995 May run,with PG 13513-489 as the primary tar ...
IAU-Perraut-2013 - Putting A Stars into Context
... IAU Conference « Putting A Stars into Context” Moscow, 2013 June 3rd ...
... IAU Conference « Putting A Stars into Context” Moscow, 2013 June 3rd ...
WHAT MAKES A STAR SO SPECIAL Abstract
... 1. The teacher introduces the physical characteristics of stars and the spectral classification to the students (you can use the information from the Introduction section as a supplement to the lesson about Star characteristics in the textbook you are using). 2. The teacher gives every student an en ...
... 1. The teacher introduces the physical characteristics of stars and the spectral classification to the students (you can use the information from the Introduction section as a supplement to the lesson about Star characteristics in the textbook you are using). 2. The teacher gives every student an en ...
Compare Star Catalogues - Asteroid Occultation Predictions
... checked. See comments below about star catalogue issues. To retrieve and plot the data, click Get and show position.It will take a few seconds to retrieve the data from Vizier. When the search is complete, the list of results will have a line stating '*** Search complete ***'. The results will appea ...
... checked. See comments below about star catalogue issues. To retrieve and plot the data, click Get and show position.It will take a few seconds to retrieve the data from Vizier. When the search is complete, the list of results will have a line stating '*** Search complete ***'. The results will appea ...
NGC 6231: a young open cluster under X-rays
... • There is no spatial trends between the cTTs and the wTTs • There is no very significant difference in their ages • Star formation in NGC 6231 was most probably not a punctual event • Formation scenario is compatible with the coalescence model for massive star formation 20-Dec-2006 ...
... • There is no spatial trends between the cTTs and the wTTs • There is no very significant difference in their ages • Star formation in NGC 6231 was most probably not a punctual event • Formation scenario is compatible with the coalescence model for massive star formation 20-Dec-2006 ...
Candidate star clusters toward the inner Milky Way discovered on
... optical, stacking multiple epochs as carried out in this work will generate deep images in the Milky Way. For simplicity, we ensured homogeneity by applying our algorithm to only one pawprint from one of the 348 VVV survey tiles, referred to in VVV as b201. There were no known clusters or cluster ca ...
... optical, stacking multiple epochs as carried out in this work will generate deep images in the Milky Way. For simplicity, we ensured homogeneity by applying our algorithm to only one pawprint from one of the 348 VVV survey tiles, referred to in VVV as b201. There were no known clusters or cluster ca ...
here - NASA/IPAC Extragalactic Database
... be called spectroscopically an O4 V. This includes any star with a mass from ∼35M⊙ to ∼85M⊙. There are a few other caveats that need to be kept in mind when talking about the main-sequence evolution of massive stars. First, the luminosity class (“I” vs “V”, say) of O-type stars depends primarily on ...
... be called spectroscopically an O4 V. This includes any star with a mass from ∼35M⊙ to ∼85M⊙. There are a few other caveats that need to be kept in mind when talking about the main-sequence evolution of massive stars. First, the luminosity class (“I” vs “V”, say) of O-type stars depends primarily on ...
Colloquial Jakartan Indonesian
... record their navigational strategies. His resulting book, We, the Navigators (1972),2 is the most complete record we are likely to get of this body of knowledge, rapidly disappearing with the increased presence of motorised boats and Western navigational technology. He was also at pains to record, i ...
... record their navigational strategies. His resulting book, We, the Navigators (1972),2 is the most complete record we are likely to get of this body of knowledge, rapidly disappearing with the increased presence of motorised boats and Western navigational technology. He was also at pains to record, i ...
![arXiv:1705.00964v1 [astro-ph.GA] 2 May 2017](http://s1.studyres.com/store/data/013011793_1-8f89fb3e8b5cd5cf78613aebb3c8e2a5-300x300.png)
Wolf-Rayet Stars
... production of low mass stars, and the short evolutionary lifetime of W-R stars, which is only a few ×105 years. Their rarity belies their importance. All stars more massive than approximately 25 M (for solar metalicity) pass through a W-R phase. Further, over the lifetime of a galaxy, W-R stars (an ...
... production of low mass stars, and the short evolutionary lifetime of W-R stars, which is only a few ×105 years. Their rarity belies their importance. All stars more massive than approximately 25 M (for solar metalicity) pass through a W-R phase. Further, over the lifetime of a galaxy, W-R stars (an ...
Study of the X-ray Source Population and the Dark Matter
... Owing to the large effective area, large field of view, and high spatial and time resolution, the Wide Field Imager of the Athena Xray Observatory will make it possible to study X-ray sources down to very low flux limits. In Draco dSph, e.g., we will be able to observe X-ray sources with luminositie ...
... Owing to the large effective area, large field of view, and high spatial and time resolution, the Wide Field Imager of the Athena Xray Observatory will make it possible to study X-ray sources down to very low flux limits. In Draco dSph, e.g., we will be able to observe X-ray sources with luminositie ...
Early-type stars in the core of the young open cluster Westerlund 2
... were bias-subtracted, flat-fielded, sky-subtracted, wavelengthcalibrated and normalized using the software developed at ESO. The S/N ratios of the calibrated spectra ranged between 60 and 150 for the faintest and brightest sources respectively, with an average of ∼ 100 for a V = 14.5 star. Sin ...
... were bias-subtracted, flat-fielded, sky-subtracted, wavelengthcalibrated and normalized using the software developed at ESO. The S/N ratios of the calibrated spectra ranged between 60 and 150 for the faintest and brightest sources respectively, with an average of ∼ 100 for a V = 14.5 star. Sin ...
Cygnus (constellation)
Cygnus /ˈsɪɡnəs/ is a northern constellation lying on the plane of the Milky Way, deriving its name from the Latinized Greek word for swan. The swan is one of the most recognizable constellations of the northern summer and autumn, it features a prominent asterism known as the Northern Cross (in contrast to the Southern Cross). Cygnus was among the 48 constellations listed by the 2nd century astronomer Ptolemy, and it remains one of the 88 modern constellations.Cygnus contains Deneb, one of the brightest stars in the night sky and one corner of the Summer Triangle, as well as some notable X-ray sources and the giant stellar association of Cygnus OB2. One of the stars of this association, NML Cygni, is one of the largest stars currently known. The constellation is also home to Cygnus X-1, a distant X-ray binary containing a supergiant and unseen massive companion that was the first object widely held to be a black hole. Many star systems in Cygnus have known planets as a result of the Kepler Mission observing one patch of the sky, the patch is the area around Cygnus. In addition, most of the eastern part of Cygnus is dominated by the Hercules–Corona Borealis Great Wall, a giant galaxy filament that is the largest known structure in the observable universe; covering most of the northern sky.