No Slide Title
... Would you weigh more or less on a white dwarf compared to what you weigh here on Earth? a) more b) less c) this is a trick question; actually, I would weight exactly the same on a white dwarf because of its size. How much more? M=300,000 times the mass of the Earth R= radius of the Earth ...
... Would you weigh more or less on a white dwarf compared to what you weigh here on Earth? a) more b) less c) this is a trick question; actually, I would weight exactly the same on a white dwarf because of its size. How much more? M=300,000 times the mass of the Earth R= radius of the Earth ...
Strong Field Dissociation and Ionization of H2
... include processes such as the above-threshold ionization (ATI) [2], where an atom or a molecule absorbs more photons than the minimum required to ionize; the abovethreshold dissociation (ATD) [3, 4], where a molecule absorbs more photons than the minimum required to dissociate; above-threshold Coulo ...
... include processes such as the above-threshold ionization (ATI) [2], where an atom or a molecule absorbs more photons than the minimum required to ionize; the abovethreshold dissociation (ATD) [3, 4], where a molecule absorbs more photons than the minimum required to dissociate; above-threshold Coulo ...
CV - iucaa
... • “Time domain science with Indian telescopes”, Caltech, August 2013 • “Building X-ray Telescopes”, IISc, April 2013 Publications • Singer, L. P., Kasliwal, M. M., Cenko, S. B., et al. The Needle in the 100 deg2 Haystack: Uncovering Afterglows of Fermi GRBs with the Palomar Transient Factory. ArXiv ...
... • “Time domain science with Indian telescopes”, Caltech, August 2013 • “Building X-ray Telescopes”, IISc, April 2013 Publications • Singer, L. P., Kasliwal, M. M., Cenko, S. B., et al. The Needle in the 100 deg2 Haystack: Uncovering Afterglows of Fermi GRBs with the Palomar Transient Factory. ArXiv ...
Dark matter, neutron stars and strange quark matter
... bag constant. For each pair of curves, the lower line is for B 1/4 = 145 MeV and the upper line is for B 1/4 = 170 MeV. For a typical baryonic density of ∼ 3nA,0 , a lower ...
... bag constant. For each pair of curves, the lower line is for B 1/4 = 145 MeV and the upper line is for B 1/4 = 170 MeV. For a typical baryonic density of ∼ 3nA,0 , a lower ...
UNIVERSITY OF CAMBRIDGE INTERNATIONAL
... (b) A student designs a sensing unit for temperature change. A 4 V supply, a fixed resistor of resistance 2.5 kΩ and a thermistor are available. The thermistor has resistance 3.0 kΩ at 6 °C and resistance 1.8 kΩ at 20 °C. Complete the circuit diagram of Fig. 9.2 to show how the resistor and the ther ...
... (b) A student designs a sensing unit for temperature change. A 4 V supply, a fixed resistor of resistance 2.5 kΩ and a thermistor are available. The thermistor has resistance 3.0 kΩ at 6 °C and resistance 1.8 kΩ at 20 °C. Complete the circuit diagram of Fig. 9.2 to show how the resistor and the ther ...
The Nuclear Equation of State and Neutron Star Masses
... Other crucial properties that are important for understanding the structure and evolution of neutron stars, such as radii and surface temperatures, can be estimated in a few cases from optical and X-ray observations of cooling neutron stars as well as from X-ray bursts and flares occurring on neutron ...
... Other crucial properties that are important for understanding the structure and evolution of neutron stars, such as radii and surface temperatures, can be estimated in a few cases from optical and X-ray observations of cooling neutron stars as well as from X-ray bursts and flares occurring on neutron ...
PRESPEC – towards gamma-ray spectroscopy of exotic nuclei at FAIR
... Where does the nuclear chart end? ...
... Where does the nuclear chart end? ...
P Cygni Profiles of Molecular Lines Toward Arp 220 Nuclei
... 2005), as well as models of HCO+ enhancement in protostellar outflow shocks (Rawlings et al. 2004). The absorbing gas will have a depth on the order of 1–10 pc if its density is at the CO(3–2) critical density of 104 cm−3 . The actual absorbing material can be distributed over a longer length if it ...
... 2005), as well as models of HCO+ enhancement in protostellar outflow shocks (Rawlings et al. 2004). The absorbing gas will have a depth on the order of 1–10 pc if its density is at the CO(3–2) critical density of 104 cm−3 . The actual absorbing material can be distributed over a longer length if it ...
Terzan 5`s Pulsars Fastest
... o The fast rotation of Ter5ad constrains its radius to be < 16 km, assuming its mass is less than 2 Msun (Fig 1). o The spin rate of Ter5ad is also an important input for models that propose gravitional radiation as a mechanism for limiting the rotation rate of neutron stars [10,11]. o The difficult ...
... o The fast rotation of Ter5ad constrains its radius to be < 16 km, assuming its mass is less than 2 Msun (Fig 1). o The spin rate of Ter5ad is also an important input for models that propose gravitional radiation as a mechanism for limiting the rotation rate of neutron stars [10,11]. o The difficult ...
Lecture 39: Early Universe Test 3 overview 11/21
... • Neutron’s mass is slightly more than proton’s mass • neutrons decay, lifetime of 15 minutes • If flip n and p mass then protons decay m p 938.3 MeV / c ...
... • Neutron’s mass is slightly more than proton’s mass • neutrons decay, lifetime of 15 minutes • If flip n and p mass then protons decay m p 938.3 MeV / c ...
mats project at fair
... the buffer gas and to prepare the cooled ions for the precision trap B4 or for a detector trap placed in the second uniform part of the same magnet as the preparatory trap. The task of the detector trap should be in-trap spectroscopy. In order to increase considerably the precision of measurements, ...
... the buffer gas and to prepare the cooled ions for the precision trap B4 or for a detector trap placed in the second uniform part of the same magnet as the preparatory trap. The task of the detector trap should be in-trap spectroscopy. In order to increase considerably the precision of measurements, ...
Acceleration and radiation of ultra
... the acceleration process at an epoch where the redshift is z 1 and we can neglect the evolution of the CMBR. Moreover, as discussed in Kang et al. (1996), the higher temperature and energy density of the CMBR at high redshifts inhibits the acceleration of protons to ultra-high energies at an early ...
... the acceleration process at an epoch where the redshift is z 1 and we can neglect the evolution of the CMBR. Moreover, as discussed in Kang et al. (1996), the higher temperature and energy density of the CMBR at high redshifts inhibits the acceleration of protons to ultra-high energies at an early ...
Nuclear drip line
In nuclear physics, the boundaries for nuclear particle-stability are called drip lines. Atomic nuclei contain both protons and neutrons—the number of protons defines the identity of that element (ie, carbon always has 6 protons), but the number of neutrons within that element may vary (carbon-12 and its isotope carbon-13, for example). The number of isotopes each element may have is visually represented by plotting boxes, each of which represents a unique nuclear species, on a graph with the number of neutrons increasing on the abscissa (X axis) and number of protons increasing along the ordinate (Y axis). The resulting chart is commonly referred to as the table of nuclides, and is to nuclear physics what the periodic table of the elements is to chemistry.An arbitrary combination of protons and neutrons does not necessarily yield a stable nucleus. One can think of moving up and/or to the right across the nuclear chart by adding one type of nucleon (i.e. a proton or neutron, both called nucleons) to a given nucleus. However, adding nucleons one at a time to a given nucleus will eventually lead to a newly formed nucleus that immediately decays by emitting a proton (or neutron). Colloquially speaking, the nucleon has 'leaked' or 'dripped' out of the nucleus, hence giving rise to the term ""drip line"". Drip lines are defined for protons, neutrons, and alpha particles, and these all play important roles in nuclear physics. The nucleon drip lines are at the extreme of the proton-to-neutron ratio: at p:n ratios at or beyond the driplines, no stable nuclei can exist. The location of the neutron drip line is not well known for most of the nuclear chart, whereas the proton and alpha driplines have been measured for a wide range of elements. The nucleons drip out of such unstable nuclei for the same reason that water drips from a leaking faucet: in the water case, there is a lower potential available that is great enough to overcome surface tension and so produces a droplet; in the case of nuclei, the emission of a particle from a nucleus, against the strong nuclear force, leaves the total potential of the nucleus and the emitted particle in a lower state. Because nucleons are quantized, only integer values are plotted on the table of isotopes; this indicates that the drip line is not linear but instead looks like a step function up close.