LEO - nina`s Senior project
... Stars-Algieba • Algieba – γ Leonis (Gamma Leonis) -Gamma Leonis is a double star in Leo. Its traditional name, Algieba or Al Gieba, comes from the Arabic Al-Jabhah, which means “the forehead.” The star is sometimes also known by its Latin name, Juba.Algieba is composed of a giant star with the spec ...
... Stars-Algieba • Algieba – γ Leonis (Gamma Leonis) -Gamma Leonis is a double star in Leo. Its traditional name, Algieba or Al Gieba, comes from the Arabic Al-Jabhah, which means “the forehead.” The star is sometimes also known by its Latin name, Juba.Algieba is composed of a giant star with the spec ...
Word - El Camino College
... To their credit, the astronomers involved are also clear about this in their paper announcing the discovery. This is a carefully done observations, and they are appropriately careful in their announcement. But if it’s true… WOW. This would be the second planet ever seen directly in an image, and the ...
... To their credit, the astronomers involved are also clear about this in their paper announcing the discovery. This is a carefully done observations, and they are appropriately careful in their announcement. But if it’s true… WOW. This would be the second planet ever seen directly in an image, and the ...
Why Star Positions?
... from the star itself, and not that due to other effects like the Earth’s rotation. It also reminds us that what has been measured is an angular shift over time, and not the actual speed of the star through space. The two are closely related, but the distinction is important. What we see is simply th ...
... from the star itself, and not that due to other effects like the Earth’s rotation. It also reminds us that what has been measured is an angular shift over time, and not the actual speed of the star through space. The two are closely related, but the distinction is important. What we see is simply th ...
Document
... New breakthrough is expected after the launch of GLAST. Several sources have been detected in the TeV range by ground-based gamma-ray telescopes. All of them, except M87, are BL Lacs at z<0.2 (more percisely, to high-frequency-peaked BL Lac – HBL). ...
... New breakthrough is expected after the launch of GLAST. Several sources have been detected in the TeV range by ground-based gamma-ray telescopes. All of them, except M87, are BL Lacs at z<0.2 (more percisely, to high-frequency-peaked BL Lac – HBL). ...
Available online www.jsaer.com Journal of Scientific and
... A retrospect of literatures on stars concerning their energy creation, colours and formation A lot of research literatures have been published about stars. This section is a retrospective light of existing star literatures on their energy creation, colours and formation. Energy (light) creation by s ...
... A retrospect of literatures on stars concerning their energy creation, colours and formation A lot of research literatures have been published about stars. This section is a retrospective light of existing star literatures on their energy creation, colours and formation. Energy (light) creation by s ...
2004 Term 1 January
... devised their material sample not from a collection of tiny rods and split rings mounted on boards, as was the case with previously reported negative-refraction materials. Instead they used a YVO4 bicrystal. Negative-refraction materials are also called "left handed materials," or LHM, because they ...
... devised their material sample not from a collection of tiny rods and split rings mounted on boards, as was the case with previously reported negative-refraction materials. Instead they used a YVO4 bicrystal. Negative-refraction materials are also called "left handed materials," or LHM, because they ...
Spectral Line Access
... Atomic lines: NIST DBs, Kurucz's CD-ROM, Atomic Line List of P. Van Hoof, TOPbase, Kelly Atomic Line DB, VALD, MCHF/MCDHF Collection, D.R.E.A.M, ...
... Atomic lines: NIST DBs, Kurucz's CD-ROM, Atomic Line List of P. Van Hoof, TOPbase, Kelly Atomic Line DB, VALD, MCHF/MCDHF Collection, D.R.E.A.M, ...
ATOMIC EMISSION SPECTROMETRY
... sources. The spectra derived from low-energy sources such as flames are simpler than those from electrical discharges, although the temperature of flames and furnaces (2000–4000 K) is inadequate to excite many of the elements. Nevertheless, flame emission spectrometry is widely used for the determinati ...
... sources. The spectra derived from low-energy sources such as flames are simpler than those from electrical discharges, although the temperature of flames and furnaces (2000–4000 K) is inadequate to excite many of the elements. Nevertheless, flame emission spectrometry is widely used for the determinati ...
Exercise Solutions
... by excitations from the third quantum level (Paschen transitions to the continuum; see Exercise 2.10). The third quantum level in hydrogen is at 12.1 eV relative to the ground state, so the minimum energy for a bound–free transition from the n D 3 level is Emin D 13:6 12:1 D 1:5 eV (since 13.6 eV ar ...
... by excitations from the third quantum level (Paschen transitions to the continuum; see Exercise 2.10). The third quantum level in hydrogen is at 12.1 eV relative to the ground state, so the minimum energy for a bound–free transition from the n D 3 level is Emin D 13:6 12:1 D 1:5 eV (since 13.6 eV ar ...
metamorphosis of an aspheric Type Ib explosion
... never been detected in pre-explosion images. So, to understand the nature of their progenitors and the characteristics of the explosions, investigation of proximate events is necessary. Here we present the results of multiwavelength observations of Type Ib SN 2007uy in the nearby (∼29.5 Mpc) galaxy ...
... never been detected in pre-explosion images. So, to understand the nature of their progenitors and the characteristics of the explosions, investigation of proximate events is necessary. Here we present the results of multiwavelength observations of Type Ib SN 2007uy in the nearby (∼29.5 Mpc) galaxy ...
astronomy powerpoint
... motion of the stars, but rises 50 minutes later each day and shifts 13° eastward each day compared to the background field of stars. The revolution of the moon around the Earth follows an elliptical shape and has a period of 27.32 days. The revolution of the moon is tilted about 5° from Earth’s ...
... motion of the stars, but rises 50 minutes later each day and shifts 13° eastward each day compared to the background field of stars. The revolution of the moon around the Earth follows an elliptical shape and has a period of 27.32 days. The revolution of the moon is tilted about 5° from Earth’s ...
First Problem Set
... †9. A burst of muons is produced by a cosmic ray interacting in the upper atmosphere. They travel towards the Earth’s surface with an average speed of 0.99c. If 1% of the burst survive to reach ground level, estimate the height of the burst and calculate the distance as measured in the muon’s frame. ...
... †9. A burst of muons is produced by a cosmic ray interacting in the upper atmosphere. They travel towards the Earth’s surface with an average speed of 0.99c. If 1% of the burst survive to reach ground level, estimate the height of the burst and calculate the distance as measured in the muon’s frame. ...
Slide 1
... the stars in the image of NGC104 above) indicates that they have similar chemical compositions and similar ages. This makes them the simplest systems to use to test theoretical models of star formation and evolution. * Furthermore, globular clusters are some of the oldest stellar systems known and t ...
... the stars in the image of NGC104 above) indicates that they have similar chemical compositions and similar ages. This makes them the simplest systems to use to test theoretical models of star formation and evolution. * Furthermore, globular clusters are some of the oldest stellar systems known and t ...
mslien~1
... Out of deep images & with the detection 20 of stars on 5 level Succeeded to detected very faint (low mass) stars ...
... Out of deep images & with the detection 20 of stars on 5 level Succeeded to detected very faint (low mass) stars ...
Optical Activity - Chemistry With BT
... A substance is optically active if it rotates the plane of polarized light. In order for a substance to exhibit optical activity, it must be chiral and one enantiomer must be present in excess of the other. ...
... A substance is optically active if it rotates the plane of polarized light. In order for a substance to exhibit optical activity, it must be chiral and one enantiomer must be present in excess of the other. ...
Young`s Double Slits
... on the zero position on the ruled screen at the other end. Now, place the slide saddle on the track in front of the beam, so that a diffraction pattern appears on the screen. Note the positions of the two saddles, and deduce their separation. Measure the separation between adjacent maxima on t ...
... on the zero position on the ruled screen at the other end. Now, place the slide saddle on the track in front of the beam, so that a diffraction pattern appears on the screen. Note the positions of the two saddles, and deduce their separation. Measure the separation between adjacent maxima on t ...
WASP-12b: THE HOTTEST TRANSITING
... in the same way as described above for the Tenagra data, and the resulting out-of-eclipse light curve has 2.5 mmag precision. The z-band and B-band transit light curves obtained via follow-up photometry are plotted in Figure 2. 2.3. SOPHIE Spectroscopy High-resolution spectroscopy of WASP-12 was obt ...
... in the same way as described above for the Tenagra data, and the resulting out-of-eclipse light curve has 2.5 mmag precision. The z-band and B-band transit light curves obtained via follow-up photometry are plotted in Figure 2. 2.3. SOPHIE Spectroscopy High-resolution spectroscopy of WASP-12 was obt ...
$doc.title
... 2048×2048 pixels corresponding to 4.10 ×4.10 on the sky. The instrument was in longslit mode with a slit width of 1.500 using Grism 14 - resulting in a wavelength range of λλ3095 − 5085 Å and a grating of 600 lines mm−1 and a dispersion of 1 Å pixel−1 yielding a wavelength range of λλ6000 − 7150 Å. ...
... 2048×2048 pixels corresponding to 4.10 ×4.10 on the sky. The instrument was in longslit mode with a slit width of 1.500 using Grism 14 - resulting in a wavelength range of λλ3095 − 5085 Å and a grating of 600 lines mm−1 and a dispersion of 1 Å pixel−1 yielding a wavelength range of λλ6000 − 7150 Å. ...
Astronomical spectroscopy
Astronomical spectroscopy is the study of astronomy using the techniques of spectroscopy to measure the spectrum of electromagnetic radiation, including visible light, which radiates from stars and other hot celestial objects. Spectroscopy can be used to derive many properties of distant stars and galaxies, such as their chemical composition, temperature, density, mass, distance, luminosity, and relative motion using Doppler shift measurements.