Distant Stars Lesson Plan
... Point out that there is a wealth of additional information not included in the ‘How far away is it’ video. ...
... Point out that there is a wealth of additional information not included in the ‘How far away is it’ video. ...
Chapter 20 Review of Stars` Lifetime Review
... • None have been detected that have formed this way • Some have been found in binary systems ...
... • None have been detected that have formed this way • Some have been found in binary systems ...
What tool do astronomers use to understand the evolution of stars?
... t B M B L A 1 300 300 60 Sun's lifetime ~ 10 billion years = 1010 yr = 10 Gyr. Lifetime of 5 solar mass star is 1010 yr/60 ~ 1010/102 yr = 108 yr = 102106 yr = 100 million yr = 100 Myr This is the age of the star cluster. ...
... t B M B L A 1 300 300 60 Sun's lifetime ~ 10 billion years = 1010 yr = 10 Gyr. Lifetime of 5 solar mass star is 1010 yr/60 ~ 1010/102 yr = 108 yr = 102106 yr = 100 million yr = 100 Myr This is the age of the star cluster. ...
Link again
... Stars can form in groups called “clusters.” Open clusters are relatively young. The Pleiades formed about 100 million years ago and the gas and dust from which they formed still surrounds them. Globular clusters contain thousands of stars and are usually around 10 billion years old. Stars begin as c ...
... Stars can form in groups called “clusters.” Open clusters are relatively young. The Pleiades formed about 100 million years ago and the gas and dust from which they formed still surrounds them. Globular clusters contain thousands of stars and are usually around 10 billion years old. Stars begin as c ...
Astronomy
... Stars can form in groups called “clusters.” Open clusters are relatively young. The Pleiades formed about 100 million years ago and the gas and dust from which they formed still surrounds them. Globular clusters contain thousands of stars and are usually around 10 billion years old. Stars begin as c ...
... Stars can form in groups called “clusters.” Open clusters are relatively young. The Pleiades formed about 100 million years ago and the gas and dust from which they formed still surrounds them. Globular clusters contain thousands of stars and are usually around 10 billion years old. Stars begin as c ...
(massive) binary stars
... Rotationally-induced mixing. A substantial enhancements of surface helium and nitrogen with the rotation rate of massive stars was theoretically predicted by Meyner & Maeder (2000, A&A, 361, 101) and Heger & Langer (2000, ApJ, 544, 1016). The authors explained the effect by rotationally-induced mixi ...
... Rotationally-induced mixing. A substantial enhancements of surface helium and nitrogen with the rotation rate of massive stars was theoretically predicted by Meyner & Maeder (2000, A&A, 361, 101) and Heger & Langer (2000, ApJ, 544, 1016). The authors explained the effect by rotationally-induced mixi ...
CHP 10
... c. composed of particles that are a few millimeters in diameter. d. formed as coronal gas cools. e. formed primarily in the atmospheres of cool stars. How can the coronal gas occupy most of the space but represent only 5 percent of the mass? a. It has a much lower pressure than the other components. ...
... c. composed of particles that are a few millimeters in diameter. d. formed as coronal gas cools. e. formed primarily in the atmospheres of cool stars. How can the coronal gas occupy most of the space but represent only 5 percent of the mass? a. It has a much lower pressure than the other components. ...
Unit 3 - Lesson 8.9 Life of Stars Challenge
... These coloured Super Giants have luminosities often 1,000,000X greater than the Sun The explosive death of a star A cloud of hydrogen gas and dust in space. When the gravitational and pressure forces within the initial cloud become unbalanced, the cloud collapses and breaks into small fragments. The ...
... These coloured Super Giants have luminosities often 1,000,000X greater than the Sun The explosive death of a star A cloud of hydrogen gas and dust in space. When the gravitational and pressure forces within the initial cloud become unbalanced, the cloud collapses and breaks into small fragments. The ...
YSO/PMS disk types, time-scales and evolution from 1
... The initial sample had photometry for 1024 YSO candidates with estimated ages of 1 -10 Myrs Encompassing the timescales of disk dissipation previously observed for low mass stars and probing slightly different environments ...
... The initial sample had photometry for 1024 YSO candidates with estimated ages of 1 -10 Myrs Encompassing the timescales of disk dissipation previously observed for low mass stars and probing slightly different environments ...
The All-Seeing, All-Magnifying Eye
... seeing when you look at these faraway galaxies through this “lens.” ...
... seeing when you look at these faraway galaxies through this “lens.” ...
The Milky Way Galaxy
... To determine the rotation curve of the Galaxy, we will introduce a more convenient coordinate system, called the Galactic coordinate system. Note that the plane of the solar system is not the same as the plane of the Milky Way disk, and the Earth itself is tipped with respect to the plane of the sol ...
... To determine the rotation curve of the Galaxy, we will introduce a more convenient coordinate system, called the Galactic coordinate system. Note that the plane of the solar system is not the same as the plane of the Milky Way disk, and the Earth itself is tipped with respect to the plane of the sol ...
Untitled
... three makes the bottom of 'The Pot', now tipped on its side. Below and right of Sirius is Procyon. Low in the northern sky is a fuzzy patch of light, the Praesepe cluster, marking the shell of Cancer the Crab. Praesepe is also called the Beehive cluster, the reason obvious when it is viewed in binoc ...
... three makes the bottom of 'The Pot', now tipped on its side. Below and right of Sirius is Procyon. Low in the northern sky is a fuzzy patch of light, the Praesepe cluster, marking the shell of Cancer the Crab. Praesepe is also called the Beehive cluster, the reason obvious when it is viewed in binoc ...
www.astro.caltech.edu
... physical cause (Figure 2). The host galaxies of short-duration GRBs (those whose gamma-ray emission lasts for 2 seconds or less) observed with Keck have been localized to a completely different host-galaxy population, one with characteristically low star-formation rates and in a few cases evidence o ...
... physical cause (Figure 2). The host galaxies of short-duration GRBs (those whose gamma-ray emission lasts for 2 seconds or less) observed with Keck have been localized to a completely different host-galaxy population, one with characteristically low star-formation rates and in a few cases evidence o ...
Star Stuff
... • where the electrons are located (which energy levels) • which elements have absorption, emission lines -- an O-star has a temperature of ~50,000 K -- an A-star has a temp of ~10,000 K, enough for hydrogen to be ionized (spectral lines in the UV) -- a G-star (like our Sun) has a temperature of ~6,0 ...
... • where the electrons are located (which energy levels) • which elements have absorption, emission lines -- an O-star has a temperature of ~50,000 K -- an A-star has a temp of ~10,000 K, enough for hydrogen to be ionized (spectral lines in the UV) -- a G-star (like our Sun) has a temperature of ~6,0 ...
Lecture 16
... 1. Main Sequence: H fuses to He in core 2. Red Supergiant: H fuses to He in shell around He core 3. Helium Core Fusion: He fuses to C in core while H fuses to He in shell 4. Multiple Shell Fusion: many elements fuse in shells 5. Supernova leaves neutron star behind and creates all elements heavier t ...
... 1. Main Sequence: H fuses to He in core 2. Red Supergiant: H fuses to He in shell around He core 3. Helium Core Fusion: He fuses to C in core while H fuses to He in shell 4. Multiple Shell Fusion: many elements fuse in shells 5. Supernova leaves neutron star behind and creates all elements heavier t ...
Analyzing Spectra
... wavelengths, producing a certain pattern of dark lines. The pattern of lines can therefore be used to identify which elements are present in a star. In this activity, you will observe spectra and determine the compositions of the sun and unknown objects by comparing the dark lines in their spectra w ...
... wavelengths, producing a certain pattern of dark lines. The pattern of lines can therefore be used to identify which elements are present in a star. In this activity, you will observe spectra and determine the compositions of the sun and unknown objects by comparing the dark lines in their spectra w ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.