Calculating Radial Velocities of Low Mass Eclipsing Binaries
... occur during the eclipse of each system, and this was observed in almost every case. Notable exceptions include EBLM11 and EBLM19, whose radial velocities did not vary over time. It remains unclear why, but we can speculate that these were perhaps ...
... occur during the eclipse of each system, and this was observed in almost every case. Notable exceptions include EBLM11 and EBLM19, whose radial velocities did not vary over time. It remains unclear why, but we can speculate that these were perhaps ...
Beers_First_Stars_NIC_School
... significantly from any previously known star. This star exhibits low [α-element/Fe] ratios and large contrasts between the abundances of odd and even element pairs, such as Sc/Ti and Co/Ni. Such features have been predicted by model calculations of the nucleosynthesis associated with a pairinstabili ...
... significantly from any previously known star. This star exhibits low [α-element/Fe] ratios and large contrasts between the abundances of odd and even element pairs, such as Sc/Ti and Co/Ni. Such features have been predicted by model calculations of the nucleosynthesis associated with a pairinstabili ...
August 2014 Saguaro Skies
... Aquila, Cygnus and Lacerta. Beginning with the western most, in Aquila, is the planetary nebula NGC6804 that is rather faint but has an irregular shape. The next two are the famous Veil Nebulae, in Cygnus, and are NGC6960 the western part and NGC6992 the eastern part. The western part is bright and ...
... Aquila, Cygnus and Lacerta. Beginning with the western most, in Aquila, is the planetary nebula NGC6804 that is rather faint but has an irregular shape. The next two are the famous Veil Nebulae, in Cygnus, and are NGC6960 the western part and NGC6992 the eastern part. The western part is bright and ...
Document
... Venn & Lambert (2008) have argued that this may not be the case. Peculiar stars such as post AGB stars and l Boo stars have iron abundances as low as [Fe/H] ~ –5. These are thought to be due to the separation of gas and dust beyond the stellar surface followed by an accretion of the dust-depleted g ...
... Venn & Lambert (2008) have argued that this may not be the case. Peculiar stars such as post AGB stars and l Boo stars have iron abundances as low as [Fe/H] ~ –5. These are thought to be due to the separation of gas and dust beyond the stellar surface followed by an accretion of the dust-depleted g ...
CHP 15
... a. I & III b. I & IV c. II & III d. II & IV e. I, III, & IV Radio maps of our galaxy show spiral arms because the a. arms have high Doppler shifts. b. gas in the spiral arms is hot enough to emit photons. c. dust in spiral arms is more dense than it is between the spiral arms. d. gas in spiral arms ...
... a. I & III b. I & IV c. II & III d. II & IV e. I, III, & IV Radio maps of our galaxy show spiral arms because the a. arms have high Doppler shifts. b. gas in the spiral arms is hot enough to emit photons. c. dust in spiral arms is more dense than it is between the spiral arms. d. gas in spiral arms ...
star - Cloudfront.net
... the region of space around them. 2. Although the stars that make up a pattern appear to be close together, they are not all the same distance from Earth. ...
... the region of space around them. 2. Although the stars that make up a pattern appear to be close together, they are not all the same distance from Earth. ...
norfolk skies - Norfolk Astronomical Society
... method described above. The nebula forms the apex of a triangle with two stars of equal brightness. Good luck on this difficult object. NGC 2327 - An interesting nebula extending north from a faint double star. It reminds me of the more famous NGC 2261 in Monocerous (Hubble’s Variable Nebula) becaus ...
... method described above. The nebula forms the apex of a triangle with two stars of equal brightness. Good luck on this difficult object. NGC 2327 - An interesting nebula extending north from a faint double star. It reminds me of the more famous NGC 2261 in Monocerous (Hubble’s Variable Nebula) becaus ...
Star Formation in Our Galaxy - Wiley-VCH
... this spectral regime comes mainly from dust heated to roughly 100 K. The fact that even this modest temperature is maintained over such an extended region demands the presence of many stars of high intrinsic luminosity. Returning to the 12 C16 O map of Figure 1.2, we see that several areas associate ...
... this spectral regime comes mainly from dust heated to roughly 100 K. The fact that even this modest temperature is maintained over such an extended region demands the presence of many stars of high intrinsic luminosity. Returning to the 12 C16 O map of Figure 1.2, we see that several areas associate ...
Document
... And to complicate matters even further, most spectral synthesis is for 1-D plane parallel models with no true velocity fields. Work by Apslund and ...
... And to complicate matters even further, most spectral synthesis is for 1-D plane parallel models with no true velocity fields. Work by Apslund and ...
Stellar Evolution
... B-star spectrum; Si II, Mn II, Cr II, Eu II, Sr II are strong. H lines strong, Ca II H & K strengthen toward later type. A-star spectrum; Si II, Mn II, Cr II, Eu II, Sr II are strong. A-star spectrum + Fe lines unusually strong. Metals, H lines weaken, Ca II strengthen — emission “bumps” appear in H ...
... B-star spectrum; Si II, Mn II, Cr II, Eu II, Sr II are strong. H lines strong, Ca II H & K strengthen toward later type. A-star spectrum; Si II, Mn II, Cr II, Eu II, Sr II are strong. A-star spectrum + Fe lines unusually strong. Metals, H lines weaken, Ca II strengthen — emission “bumps” appear in H ...
13.1 Introduction 13.2 The Red Giant Branch
... degenerate. In detailed models, a series of smaller flashes follows the main He flash (see Figure 13.3) for ∼ 1.5 Myr, before degeneracy in the centre is completely lifted and further He burning proceeds stably in a convective core. This is the situation when stars with a non-degenerate core reach T ...
... degenerate. In detailed models, a series of smaller flashes follows the main He flash (see Figure 13.3) for ∼ 1.5 Myr, before degeneracy in the centre is completely lifted and further He burning proceeds stably in a convective core. This is the situation when stars with a non-degenerate core reach T ...