992 research outputs found
Acoustic confinement and Stimulated Brillouin Scattering in integrated optical waveguides
We examine the effect of acoustic mode confinement on Stimulated Brillouin
Scattering in optical waveguides that consist of a guiding core embedded in a
solid substrate. We find that SBS can arise due to coupling to acoustic modes
in three different regimes. First, the acoustic modes may be guided by total
internal reflection; in this case the SBS gain depends directly on the degree
of confinement of the acoustic mode in the core, which is in turn determined by
the acoustic V-parameter. Second, the acoustic modes may be leaky, but may
nevertheless have a sufficiently long lifetime to have a large effect on the
SBS gain; the lifetime of acoustic modes in this regime depends not only on the
contrast in acoustic properties between the core and the cladding, but is also
highly dependent on the waveguide dimensions. Finally SBS may occur due to
coupling to free modes, which exist even in the absence of acoustic
confinement; we find that the cumulative effect of coupling to these
non-confined modes results in significant SBS gain. We show how the different
acoustic properties of core and cladding lead to these different regimes, and
discuss the feasibility of SBS experiments using different material systems
The nature of the progenitor of the Type II-P supernova 1999em
We present high quality ground-based VRI images of the site of the Type II-P
SN1999em (in NGC1637) taken before explosion, which were extracted from the
CFHT archive. We determine a precise position of the SN on these images to an
accuracy of 0.17''. The host galaxy is close enough (7.5 +/- 0.5 Mpc) that the
bright supergiants are resolved as individual objects, however we show that
there is no detection of an object at the SN position before explosion that
could be interpreted as the progenitor star. By determining the sensitivity
limits of the VRI data, we derive bolometric luminosity limits for the
progenitor. Comparing these to standard stellar evolutionary tracks which trace
evolution up to the point of core carbon ignition, we initially derive an upper
mass limit of approximately 12M_sol. However we present evolutionary
calculations that follow 7-12M_sol stars throughout their C-burning lifetime
and show that we can restrict the mass of the progenitor even further. Our
calculations indicate that progenitors initially of 8-10M_sol, undergoing
expected mass loss, can also be excluded because a second dredge up sends them
to somewhat higher luminosities than a star of initially 12M_sol. These results
limit the progenitor's initial main-sequence mass to a very narrow range of 12
+/- 1 M_sol. We discuss the similarities between the Type II-P SNe 1999em and
1999gi and their progenitor mass limits, and suggest that SN Type II-P
originate only in intermediate mass stars of 8-12M_sol, which are in the red
supergiant region and that higher mass stars produce the other Type II
sub-types. (Abridged).Comment: Replaced with accepted version to appear in ApJ, 30 pages, inc. 6
figure
Binary coalescence from case A evolution -- mergers and blue stragglers
We constructed some main-sequence mergers from case A binary evolution and
studied their characteristics via Eggleton's stellar evolution code. Both total
mass and orbital angular momentum are conservative in our binary evolutions.
Some mergers might be on the left of the ZAMS as defined by normal surface
composition on a CMD because of enhanced surface helium content. The study also
shows that central hydrogen content of the mergers is independent of mass. As a
consequence, we fit the formula of magnitude and B-V of the mergers when they
return back to thermal equilibrium with maximum error 0.29 and 0.037,
respectively. Employing the consequences above, we performed Monte Carlo
simulations to examine our models in NGC 2682 and NGC 2660. In NGC 2682, binary
mergers from our models cover the region with high luminosity, but its
importance is much less than that of AML. Our results are well-matched to the
observations of NGC2660 if there is about 0.5Mo of mass loss in the merger
process.Comment: 14 pages, 12 figures. accepted by MNRA
Impact of nonlinear loss on Stimulated Brillouin Scattering
We study the impact of two-photon absorption (2PA) and fifth-order nonlinear
loss such as 2PA-induced free-carrier absorption in semiconductors on the
performance of Stimulated Brillouin Scattering devices. We formulate the
equations of motion including effective loss coefficients, whose explicit
expressions are provided for numerical evaluation in any waveguide geometry. We
find that 2PA results in a monotonic, algebraic relationship between
amplification, waveguide length and pump power, whereas fifth-order losses lead
to a non-monotonic relationship. We define a figure of merit for materials and
waveguide designs in the presence of fifth-order losses. From this, we
determine the optimal waveguide length for the case of 2PA alone and upper
bounds for the total Stokes amplification for the case of 2PA as well as
fifth-order losses. The analysis is performed analytically using a small-signal
approximation and is compared to numerical solutions of the full nonlinear
modal equations
Power limits and a figure of merit for stimulated Brillouin scattering in the presence of third and fifth order loss
We derive a set of design guidelines and a figure of merit to aid the
engineering process of on-chip waveguides for strong Stimulated Brillouin
Scattering (SBS). To this end, we examine the impact of several types of loss
on the total amplification of the Stokes wave that can be achieved via SBS. We
account for linear loss and nonlinear loss of third order (two-photon
absorption, 2PA) and fifth order, most notably 2PA-induced free carrier
absorption (FCA). From this, we derive an upper bound for the output power of
continuous-wave Brillouin-lasers and show that the optimal operating conditions
and maximal realisable Stokes amplification of any given waveguide structure
are determined by a dimensionless parameter involving the
SBS-gain and all loss parameters. We provide simple expressions for optimal
pump power, waveguide length and realisable amplification and demonstrate their
utility in two example systems. Notably, we find that 2PA-induced FCA is a
serious limitation to SBS in silicon and germanium for wavelengths shorter than
2200nm and 3600nm, respectively. In contrast, three-photon absorption is of no
practical significance
An all-optical buffer based on temporal cavity solitons operating at 10 Gb/s
We demonstrate the operation of an all-optical buffer based on temporal
cavity solitons stored in a nonlinear passive fiber ring resonator. Unwanted
acoustic interactions between neighboring solitons are suppressed by modulating
the phase of the external laser driving the cavity. A new locking scheme is
presented that allows the buffer to operate with an arbitrarily large number of
cavity solitons in the loop. Experimentally, we are able to demonstrate the
storage of 4536 bits of data, written all-optically into the fiber ring at 10
Gb/s, for 1 minute.Comment: 5 pages, 4 figure
An evolutionary study of the pulsating subdwarf B eclipsing binary PG1336-018 (NY Vir)
The formation of subdwarf B (sdB) stars is not well understood within the
current framework of stellar single and binary evolution. In this study, we
focus on the formation and evolution of the pulsating sdB star in the very
short-period eclipsing binary PG1336-018. We aim at refining the formation
scenario of this unique system, so that it can be confronted with observations.
We probe the stellar structure of the progenitors of sdB stars in short-period
binaries using detailed stellar evolution calculations. Applying this to
PG1336-018 we reconstruct the common-envelope phase during which the sdB star
was formed. The results are interpreted in terms of the standard
common-envelope formalism (the alpha-formalism) based on the energy equation,
and an alternative description (the gamma-formalism) using the angular momentum
equation. We find that if the common-envelope evolution is described by the
alpha-formalism, the sdB progenitor most likely experienced a helium flash. We
then expect the sdB mass to be between 0.39 and 0.48 Msun, and the sdB
progenitor initial mass to be below ~2 Msun. However, the results for the
gamma-formalism are less restrictive, and a broader sdB mass range (0.3 - 0.8
Msun) is possible in this case. Future seismic mass determination will give
strong constraints on the formation of PG1336-018 and, in particular, on the CE
phase.Comment: 9 pages, 7 figures, 2 tables, accepted for publication in A&
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