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"The Principles of Improvisation" Collection is designed for use with ALL INSTRUMENTS
– strings, brass, woodwind, keyboards, percussion –
in ALL GENRES of music
– Classical, Blues, Jazz, Country, Rock, Latin, HipHop, Rap, Oriental –
for ALL musicians of ANY PLAYING ABILITY
– Beginner, Intermediate & Advanced –
when your aim is to create the improvised line.
Q: What is improvisation?
A: There are two answers.
1: a spontaneous response by a performer on a musical instrument to the chords in a given key;
2: a system of texts and charts designed to develop the ability of generating ideas on what to play improvisation.
Q: Can anyone learn to play improvisation?
A: Yes, providing you have the three prerequisites –
1: a rudimentary knowledge of music including the ability to read it;
2: an average ability to play a musical instrument;
3: an enquiring mind capable of understanding and creating new ideas.
Q: How much knowledge of music do I need to understand the books on The Improvised Line?
A: My ambition at the outset was to create a system that Blind Freddy could understand, so the answer is very little. Every situation has been catered for. You can start from scratch with book 1 – An Introduction to Improvisation or jump right in at the deep end with Books 9, 10 and 11 The Occidental, Oriental and Chromatix Handbooks. These are for the experienced players only as they are quite advanced.
Q: How long does it take to learn how to play improvisation?
A: After one lesson you will have more than enough information to create ideas for playing improvisation.
Q: How long does it take to become competent at playing improvisation?
A: In ancient Greece the philosophers who taught music (Muses) thought three years was adequate time to learn all that was known. But the reality today is it would take more than one lifetime to remember all the variables. That is not to say you should wait a lifetime to begin. Start now and go with what you know.
Better education will bring about more sophisticated statements.
Q: What is a Music Mode?
A: Put simply (and we love to do that) Modes are the scales within a scale. Hence there are only 7 modes, one for each note of the scale.
The Ionian Mode is the normal scale beginning on the 1st / Tonic / Naming note.
The Dorian Mode uses the same notes as the Ionian but begins on the 2nd / SuperTonic note.
The Phrygian Mode uses the same notes as the Ionian but begins on the 3rd / Mediant note.
The Lydian Mode uses the same notes as the Ionian but begins on the 4th / SubDominant note.
The MixoLydian Mode uses the same notes as the Ionian but begins on the 5th / Dominant note.
The Aeolian Mode uses the same notes as the Ionian but begins on the 6th / SubMediant note.
The Locrian Mode uses the same notes as the Ionian but begins on the 7th / SubTonic / Leading note.
Q: Why a secure PDF downloadable book instead of hard-cover book?
A: ebooks are convenient electronic books that can be instantly downloaded and read on any computer, laptop, tablet or smart phones. For those who prefer hard copies, you can print them from your own pc.
The bottom line is that we have chosen this format to reduce the price to you!
A traditional, hard-copy book would cost three times as much as the ebook, given the mark-up from the publisher, editing, distribution, shipping, etc.
The ebook format allows us to reach a wide range of people and provide them with an easily accessible and affordable guide to the improvised line.
Q: What makes this system better or different from other material on the subject of improvisation?
A: In four simple statements
1: The Principles of Improvisaton does not pretend to tell you the how, when or what to play.
2: All that it claims to do is to lay a solid foundation for you to develop your own ideas.
3: It concentrates on developing your ability to generate ideas for playing improvisation.
4: This is the ONLY system that offers the PROOF of what it states at every stage of development.
Q: I've been studying music for some time now, do I still need to buy Book 1?
A: Probably not, but you might need to refer to it some time in the future if you are not familiar with all aspects of jazz improvisation and creating the improvised line.
Q: Do I need to buy every book in the series to become competent at playing improvisation?
A: No, any one book in the series is enough to generate more than a lifetime of ideas on improvisation, so much so that you could become a 'modal specialist'. But would that be stereotyping?
Q: Is there any way of getting all the information without having to purchase all the books separately?
A: No. Books 2 to 8 have the complete information relevant to The Modes they are written in, which is not mentioned in the other ebooks on The Principles of Improvisation.
If your music education is well founded, and by that I mean to university level, you could get away with books 9,10 and 11 – The Occidental, Oriental and Chromatix Handbooks.
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A: With our new, fast and FULLY AUTOMATED Ordering Service you will have your personal copy of any of our eBooks within minutes. Just Select your book, Pay via PayPal then Click on the Download Link.
Q: I've done all the homework, so why am I still afraid to get up in public and have a go?
A: At some stage or another in their development everybody will have to face up to this situation. It is based on the fear that you will look like a 'big goose' playing too many bum notes. Let me reassure you, there are no wrong notes, because in a particular key, every note in the scale can be played with any chord in that scale. Plus there are numerous peripheral scales.
For example, including the natural scale there are eight others that produce the Dominant G7. All are compatible with the chords in key of C and the chords generated by the alterations. Then there are the modal scales… I shudder to think how many… there is enough evidence to convince anyone that there are no wrong notes.
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Music Improvisation An Innovative Method
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miAim (my aim) is to create a level playing field, where all who wish to reach their full potential at musical improvisation and composition, can find the most comprehensive materials to assist them with the greatest expediency to attain their goal. Improvisation will cease to be an intangible phenomenon. © Donald A Ahern
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I used to do a lot of Promotions in my Blog but I did pause them for a while. Good news is that I am back and I will be doing Post Promotions once again. Although this wouldn't be a Daily Post Promotion I would like to do at least two per Week.
I feel Rules are necessary for something like this. So here are some Rules you have to Follow.
1. Post a link to one of Your Post in the Comments Below that you think deserves more Attention.
2. Only one link Per Person will be Counted. No Multiple Entries.
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Good evening and a warm welcome to Heritage Park to the players, officials and supporters from Newton Aycliffe.
On Tuesday 19th, we visited Jarrow Roofing and the team played very well gaining a 2-1 victory and even with our slim squad we certainly went to Bedlington on Saturday confident we could do well against our second division opponents in the FA Vase. Despite going close on a number of occasions we disappointingly went down 2-0. It didn't help Colin in his preparations when another two players contacted him to say they didn't want to play for the Club. Colin did say at our recent Q & A, to our supporters who attended, that we would get some setbacks while he re-built the squad and this was certainly a setback but I am confident Colin, his management team and the players will turn things around.
Tonight's game sees us in in 15th position with 9 points from 10 games and with games in October against Morpeth, Shildon, Consett and Ryhope, all in the top 10 in the league, we certainly need to be fighting for maximum points in our coming games.
On Friday, we hosted the Middlesbrough Under 23 v Stoke City Under 23 game and as you know by now the game was halted by a fire in the ladies toilets in the main building. I would like to thank my fellow officials and our volunteers who were on duty on Friday for controlling the incident effectively and thanks to both teams, the match officials and the supporters for their patience and understanding whilst the game was halted. Many thanks also to the Fire Brigade for their quick response and skills in dealing with the fire.
One issue that occurred on Friday was that a late-comer parked his/her car at the top of the car park in the restricted area thus preventing the fire engines getting as close to the building as possible. I would urge people, even if the car par is full to consider the implications of such action. This area needs to be kept clear of vehicles for all emergency services to have access to the main building.
Apologies for the inconvenience to everyone with regard to car parking as we have lost the main car park to Murphy's Fun Fair. We know from the days when Darlington played at HP with gates of 1,000 plus that there are plenty of places to park near the stadium.


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\section{INTRODUCTION}

High velocity clouds (HVC) are atomic HI cloud complexes located at high
galactic latitudes, and moving with large velocities ($\mid V_{LSR} \mid \geq
90$ km/s) that do not match a simple model of circular rotation for our Galaxy
(see Mirabel 1981a, Bajaja \etal 1985, and Wakker \& van Woerden 1997). The
present data indicates an excess of negative-velocity (infall) HVC over
positive-velocity HVC, but the interpretation for their origin and evolution
is unclear because their distances and tangential motions are unknown. Limits
to the location of some particular clouds indicate $z$-heigths of a few
kiloparsecs (a recent detection of highly ionized HVCs indicates even larger
distances, but the relationship between ionized and neutral HVCs is unclear;
Sembach \etal 1998), setting a possible mass range of 10$^{5}$-10$^{6}$ \MSUN
\ for some of these complexes. Thus, a HVC complex moving with a speed of 100
km s$^{-1}$ has a kinetic energy of about 10$^{52-53}$ erg. This range of
values (equivalent to that from an OB association in the disk) indicate that
the bulk motion of the HVC system, and its interaction with the galactic disk,
could represent a rich source of energy and momentum for the interstellar
medium (ISM).

Observational signatures for the interactions of HVCs with galactic disks have
been claimed in our Galaxy and in some external galaxies. The best known
examples are in complexes AC and H, both located near the anticenter region
(Mirabel 1981b; Mirabel \& Morras 1990; Tamanaha 1997; Morras \etal 1998), in
the direction of the Draco Nebula (Kalberla \etal 1984; Hirth \etal 1985;
Herbstmeier \etal 1996), in M101 (van der Hulst \& Sancisi 1988), and in NGC
4631 (Rand \& Stone 1996).
These observations support the idea that HVC-galaxy collisions can have a
significant influence on the structure and energetics of the gaseous disk.
Previous 2-D and 3-D numerical simulations for collisions with $non-magnetic$
(or weakly magnetic) and $thin$ disks (\eg Tenorio-Tagle \etal 1986,1987;
Franco \etal 1988; Comer\'on \& Torra 1992; Lepine \& Duvert 1994; Rand \&
Stone 1996), indicate that the resulting ISM structures have sizes of several
hundreds of parsecs, similar to those ascribed to multi-supernova remnants,
or superbubbles, from OB associations. The colliding HVCs can sweep a great
amount of disk mass in these non-magnetic models. The resulting shocked layer
collects both the disk mass and the mass from the HVC, inducing the
formation of massive gas structures far from the midplane (Franco 1986; Alfaro
\etal 1991; Cabrera-Ca\~no \etal 1996). Moreover, the fastest moving clouds can
even drill holes through the whole gaseous disk, venting gas into the other
side of the disk. Thus, for these thin disk cases, an efficient mass
exchange can result from the interaction of the HVC system with the disk.

The HVC-disk interactions, however, can have a radically different outcome in
a disk that is thicker and more magnetized than assumed by these previous works
(see Cox 1990 and Franco \etal 1995). The transition between the main gaseous
disk and the halo is very broad and complex, with an intricate magnetic field
structure and a number of extended gas components, including dusty high-$z$
layers and the so-called ionized Reynolds layer (Hoyle \& Ellis 1963; Reynolds
1989). Using the available data at the Solar neighborhood, Boulares \& Cox
(1990; hereafter BC) have incorporated the distended gas components, along with
the vertical gradient of the magnetic field, in a model for the thick disk of
the Galaxy. They found that a time averaged hydrostatic support of the disk
requires scaleheights of about 1 kpc for both the ionized Reynolds layer and
the magnetic and cosmic ray pressures. These extended gas layers are not
unique to our Galaxy, and recent observations indicate that they are probably
common in spirals. Examples of diffuse ionized gas in external galaxies, that
seem to be analogous to the Reynolds layer in our Galaxy, are the prominent
$H_{\alpha}$ diffuse halos in NGC 891 and NGC 5775, and to a lesser extent in
NGC 4302 (Rand 1995). In particular, NGC 891 reveals $H_{\alpha}$ emission
extending up to 3 kpc above the midplane (Rand, Kulkarni \& Hester 1990), along
with other extraplanar structures such as worms (Dettmar 1990) and dusty
filaments (Howk \& Savage 1997). Also, the magnetic fields in edge-on galaxies
can be traced for several kpcs above the disk (Hummel \& Beck 1995), and dusty
filaments extending for more than 2 kpc above the plane of the host galaxy have
been observed in NGC 253 and NGC 7331 (Sofue 1987). Some of these features are
expected from the action of radiation pressure on dusty HI clouds (Franco
\etal 1991), and from the spiral density wave (Martos \& Cox 1998).

Regardless of some poorly known ISM parameters (such as the distribution and
filling factor of the hot gas), the existence of extended gas layers (neutral
or ionized) might have far reaching consequences for the structure and overall
stability of the gaseous disk. Any given parcel of gas located above the
scaleheight of the thin disk weighs more than the same material placed within
this disk. The inclusion of an extended gas layer, then, results in a disk
model with a total interstellar pressure that is higher than the previously
assumed thin disk values (this is in line with recent UV studies that indicate
that the thermal pressure near the Sun can be a factor of 8 higher than
previous estimates; Bergh\"ofer \etal 1998). The non-thermal pressure gradients
at high latitudes, along with the tension of magnetic lines, must play a
crucial role in the overall support of these extended disk structures (BC;
Zweibel 1995). The presence of a thick magnetic disk, then, should drastically
alter the results obtained with purely hydrodynamic models, or models in which
the gradients are concentrated in a thin disk with a scaleheight of about 150
pc.

In this paper, we present two dimensional simulations of HVCs colliding with
a thick disk, including both the purely hydrodynamic and the ideal
magnetohydrodynamic regimes. Magnetized models are built from an isothermal gas
distribution, in which magnetic support at high $z$-locations is crucial for
the initial equilibrium state. The models have the field lines parallel to the
galactic disk, but we consider two different line orientations: field lines
lying in the plane of motion of the HVC, and field lines that are normal to
this plane. The results with these orientations, along with those of the purely
hydrodynamic cases, allow us to isolate the effects of field tension: for lines
lying in the plane of motion, magnetic tension reverses the motion of HVC
material and creates an outflow at late times. For the case when the field
lines are perpendicular to the plane of motion, which have no tension effects,
the magnetic pressure prevents the cloud material from reaching deep into the
disk. Thus, in either case, the magnetic field does not allow any mass exchange
with the halo. In contrast, the non-magnetic cases (which demand a hot halo for
the initial equilibrium) evolve without resistance and allow mass mixing. The
results for these non-magnetic models confirm previous results, but some new
features are uncovered here. Also, the resulting gas structures are now
modified by the thicker and more pressurized nature of our models. The
evolution of impinging HVCs, with a range of approaching angles and velocities,
is followed with the MHD code ZEUS 3-D. The thick disk models are described in
the next section. Section 3 deals with the numerical treatment of the problem.
Section 4 presents our results, which are summarized and discussed in Section
5.

\section{Magnetized Disk Models}

The magnetic disk model is plane-parallel. Two forms of pressure, thermal
and magnetic, provide the support of the initial magnetohydrostatic equilibrium
state against the gravitational field provided by the disk stars. Our model
does not include cosmic-ray pressure. The density and gravitational
acceleration functions are given by:
\begin{eqnarray}
{\rho}(z) & = & \rho_0 [0.6e^{-\frac{z^2}{2(70pc)^2}}+
                 0.3e^{-\frac{z^2}{2(135 pc)^2}}
               + 0.07 e^{-\frac{z^2}{2(135 pc)^2}} \\ \nonumber
           &   & + 0.1e^{-\frac{|z|}{400 pc}}+0.03e^{-\frac{|z|}{900 pc}} ]
               \ \ \ {\rm cm}^{-3}
\end{eqnarray}
and
\begin{equation}
g(z) = 8\times 10^{-9}(1-.52e^{-\frac{|z|}{325 pc}}-.48e^{-\frac{|z|}{900 pc}}
)
       \ \ \ {\rm cm\, s}^{-2},
\end{equation}
\noindent
where the midplane gas density is $\rho_0 =2.24\times 10^{-24}$ g cm$^{-3}$.
This density distribution adequately describes the observed gas $z$-structure
in the solar vecinity, as discussed by BC. The functional form for the
gravitational acceleration $g$ is taken from Martos (1993), and provides a
good fit to the data of Bienaym\' e, Robin \& Cr\' ez\' e (1987).

The total pressure is given by $p(z) = -\int_z^{z_{ext}} \rho g \, dz$, with
the boundary condition $p(z_{ext} = $5 kpc)=0, and is numerically solved and
set equal to the sum of the thermal, $p_t=n(z)kT_{eff}$, and magnetic, $p_b =
B^2(z)/8\pi $, terms. The midplane values are taken from BC: total pressure
$p(0) =2.7\times 10^{-12}$~dyn~cm$^{-2}$ (this is 20\% higher than the thermal
pressure value derived by Bergh\"ofer \etal 1998), a magnetic field strength of
$B(0) = 5\ \mu$G, and an effective disk temperature of $T_{eff}(0)=10900$ K.
For simplicity, the magnetic model we adopt, which may be called a ``warm''
magnetic disk model, is defined by $T_{eff}(z) = T_{eff}(0)$ (independent of
$z$). Thus, the implicit sound speed of this warm model is similar to the
observed velocity dispersion of the main HI cloud component, $\sim 8$ km
s$^{-1}$. The total magnetic field intensity at midplane adopted in this model
includes contributions of the orderly (with a strength of $\sim 2 \ \mu$G) and
the dominant random component values (see Heiles 1996). This results in a
moderate field value for a spiral galaxy, $5\ \mu$G, because an average total
field strength of 19 $\mu$G has been derived for the disk of NGC 2276 (Hummel
\& Beck 1995). We assume magnetic field lines that are parallel to the
midplane, as indicated by data near the plane (see Valle\'e 1997), in our
initial magnetohydrostatic states.

In the 2-D MHD regime, the adopted warm disk model is Parker unstable (Martos
\& Cox 1994) and, from a linear stability analysis for the undular mode, we
have found that the minimum growth time and the corresponding wavelength are 60
Myr and 3 kpc, respectively (Kim \etal 1999). The 2-D models indicate that the
density enhancements become clearly apparent on timescales of the order of 100
Myr (Franco \etal 1995; Santill\'an \etal 1999). The instability can be
triggered by a HVC collision (see Franco \etal 1995), but the HVC-disk
interaction evolves in shorter timescales (the clouds are completely shocked in
only a few Myr). Thus, given that the timescales for the two events are very
different, here we do not discuss the appearance of the Parker instability, and
a more complete description of the instability in a thick disk (\ie the linear
analyses and the nonlinear evolution) will be reported elsewhere (Kim \etal
1999; Santill\'{a}n \etal 1999).

These magnetic models reflect conditions in which the total pressure decreases
more slowly than the density as $z$ increases. At high $z$, the models mimic
the expected dominance of non-thermal forms of pressure, and the effective
signal speed is high. As a consequence, the compressibility of the plasma is
effectively controlled by the magnetic term, and the medium is ''stiff`` and
elastic (Martos \& Cox 1998). The thermodynamic regime of the runs, isothermal
or adiabatic, can only alter that character to a certain extent, but the
assumed magnetic field geometry will certainly affect the response to any
interaction (further details of the properties of this thick, magnetic model
can be found in Martos 1993 and Martos \& Cox 1994). The distinction between
models with field lines in the plane of motion and perpendicular to the plane
of motion, then, corresponds to whether the magnetic tension influences the
dynamical evolution or not, respectively. Both types of magnetized models are
inititated in equilibrium and with the same $z$-distribution for the total
pressure. The total pressure distribution is shown in Figure 1a. The
corresponding $z$-variations for the Alfv\'en and maximum magnetosonic (the
quadratic sum of the Alfv\'en and sound velocities) wave speeds are shown in
Figure 1b. The magnetosonic speed is the effective signal speed for
compressional waves, and has a rapid increase inside the disk but varies
slowly, from 50 to 60 km s$^{-1}$, in a wide $z$ interval from 500 to 1500 pc.

For completness, we have considered an additional third model representing a
non-magnetic thick disk. This model maintains the same total pressure as in the
previous magnetic models. Hence, hydrostatic equilibrium determines the
temperature structure along the $z$-axis, $T(z)= \int_{z_{ext}}^z \rho g \, dz
/kn(z)$, with the density and gravity distributions described above. The
resulting temperature and sound speed distributions are shown in Figure 1c.

\section{Numerical Method}

The simulations are performed with the MHD code ZEUS-3D (version 4.2), which
solves the three dimensional system of ideal MHD equations by finite
differences on an Eulerian mesh (for a description of the code, see \cite{SNa},
1992b). The code can perform simulations in 3D but, due to computational
restrictions, here we restrict the discussion only to two dimensional
simulations. The effects of self-gravity and differential rotation of the
Galaxy are not included in the present version. The role of self-gravity is not
important at the densities considered here, but the effects due to the shear of
the galactic disk may be important during the evolution. When differential
rotation is included, there are at least two effects that may prove to be
significant for the HVC-disk collisions: first, the shear can cause distortions
in the resulting gaseous structures (\eg Olano 1982; Pal\v{o}us, Franco \&
Tenorio-Tagle 1990) and, second, it can trigger the appeareance of
magneto-rotational instabilities (\eg Chandrasekar 1960; Balbus \& Hawley 1991;
Foglizzo \& Tagger 1994).

In particular, the combined effects of the Parker and the magneto-rotational
instabilities may lead to interesting results (Foglizzo \& Tagger 1994). These
instabilities have different dynamical effects on the plasma and magnetic field
lines. The Parker instability distort the magnetic lines, generating a vertical
component from an originally horizontal field and redistributing the gas in the
disk. The magneto-rotational process stretches the field lines radially and
generates internal torques, driving radial gas flows. Depending on the initial
state, the instabilities may interfere constructively, with the vertical field
lines from the Parker mechanism feeding back onto the magneto-rotational
mechanism. In other cases, however, both processes operate in a stabilizing
manner (Foglizzo \& Tagger 1994). These issues are important and require
detailed three dimensional studies with differential rotation that,
unfortunately, are beyond our present capabilities. The 2-D results of the
present paper cannot include the galactic shear, and the 2D computational
domain lies in the plane defined by the azimuthal and vertical directions of
the Galaxy.

Our frame of reference is one in which the Galactic gas is at rest, and the
origin of our 2D Cartesian grid is the local neighborhood. The coordinates
($x$, $z$) represent distances along and perpendicular to the midplane,
respectively. The $x$-axis is anchored at a constant galactocentric radius
(\ie is quasi-azimuthal, defined by the tangent of the local field orientation
in our Galaxy; see Heiles 1994 and Valle\'e 1997), and the motion of the HVC
is always considered in the ($x$, $z$) plane. Two different setups for the
magnetic field are considered: $B$ parallel to the $x$-axis, in the plane of
motion of the HVC, and $B$ parallel to the $y$-axis, perpendicular to the plane
of motion (and no deformation of the field is introduced by the dynamics of the
gas). The $y$-direction is also defined in the midplane, but it would
correspond to the galactocentric radial vector direction.

For an efficient use of computer resources, we mostly worked with moderate
resolutions of 200$\times$200 zones, but verified that the results were not
different from those obtained in runs with resolutions of 400$\times$400 zones.
We performed runs with a variety of different sizes but, for simplicity, the
physical intervals of the simulations presented here are 3 kpc $\times$ 3 kpc
(the $z$-axis runs from -1.5 kpc to 1.5 kpc). Thus, one zone has an extent of
15 pc per dimension, or better, with our linear zoning scaling. The boundary
conditions are cyclic (periodic) in $x$, and free outflow in $z$. The
evolution was computed in both the isothermal ($\gamma = 1.01$) and adiabatic
($\gamma = 1.67$) regimes, since explicit cooling or heating functions are not
included in our numerical scheme.

For simplicity, all infalling clouds were given the same dimensions, $210\times
105$ pc (longer in the $x$ direction), and they are threaded by the magnetic
field strength corresponding to their initial locations. We performed some runs
with other cloud
sizes but, except for the sizes of the initial pertubations, the results are
similar to the ones described here. Since the evolution is followed on the
$x-z$ plane, and we have set the initial density of the clouds to
$n$=1 cm$^{-3}$, the mass and energy densities of the models were $5.0\times
10^{-25}$ g cm$^{-3}$ and $2.5\times 10^{-11}$ erg cm$^{-3}$ (this would
correspond to a cloud mass and kinetic energy of $3.5 \times 10^5$ \MSUN \ and
$3.5\times 10^{52}\  v^2_{100}$ erg, respectively, where $v_{100}$ is the cloud
velocity in units of 100 km s$^{-1}$, if we set the third dimension to the
quadratic mean of the other two).

We positioned the cloud centers at several selected heights, from 350 pc to
4050 pc, and made a series of runs with different incoming velocities and
incident angles. The velocity range spanned was from 0 to 200 km s$^{-1}$ (\ie
from free-fall to nearly the largest observed approaching velocity), and the
angles were varied from 0$^\circ$ to 60$^\circ$ with the vertical ($z$) axis.
Regardless of the initial position of the cloud, the entire cloud is
shocked in less than 3 Myr. The evolution of the interaction is fast and takes
place in a relatively small region (with dimensions of several dozens of cell
sizes). Thus, the details of the early shock structure (which depend on the
initial cloud conditions) are not resolved in our simulations (the interested
reader can find a detailed discussion of high resolution simulations for cloud
collisions in Klein \& McKee 1994 and Mac Low \etal 1994), and we focus here
only in the larger scale outcome of the impact (\ie in structures of the order
of a hundred pc or larger). A summary of the runs presented in this paper is
given in Table 1.

\section{Results}

\subsection{Non--magnetic thick disk}

As stated before, previously published calculations of HVC impacts have been
performed with a thin Galactic disk model, and most of them are perpendicular
collisions in the purely hydrodynamic regime. We start by comparing them with
our results obtained with the non-magnetic disk model described above. This
non-magnetic model requires a hotter halo and the thermal sound speed increases
rapidly inside the main disk (see Figure 1c).

Loosely speaking, the basic structures formed by the collisions are similar to
those described in previous modeling. For instance, as found in earlier works,
the sizes and shapes of the shocked layers in the disk resemble some of the HI
supershells observed by Heiles (1984) in our Galaxy. There are, however, some
clear differences with previous results, and they are mainly due to our more
extended gas distributions (\ie the structures formed at high $z$-locations are
denser, better defined, and last longer than in the thin disk cases). Also, the
resulting rear wakes are now completely formed and their morphologies and
vorticities are clearly apparent. In particular, here we see one conspicuous
structure, the tail, that has been either missed or disregarded in former
studies (this is likey due to the fact that most previous models have located
the HVC much closer to the midplane). The importance of this feature is better
appreciated in (magnetic and non-magnetic) oblique impacts, and may be one
of the possible sources of turbulence in the Reynolds' layer (see Benjamin 1998
and Tufte \etal 1998).

\subsubsection{HVC with $V_{HVC}$ = 200 km s$^{-1}$, and $\theta = 0^\circ$}

Our first example is a purely hydrodynamic simulation of a collision
perpendicular to the disk (impact angle $\theta = 0^\circ$). The evolution is
shown in the four snapshots displayed in Figure 2. The simulation is performed
in the isothermal mode and the HVC center position is located at 1250 pc from
midplane, with an initial velocity of 200 km s$^{-1}$. In all the following
figures, the density is shown in logarithmic grayscale plots and the velocity
field is indicated by arrows sized proportionally to the local speed.

The first two snapshots show the initial conditions and the shock evolution at
3.2 Myr, respectively. The impact creates a strong galactic shock directed
downwards, and a reverse shock that penetrates into the cloud. The galactic
shock tends to move radially away from the location of impact, but momentum
conservation keeps it strongest in the direction of motion of the impinging
cloud. The lateral components of the shock, then, are milder and become a sonic
perturbation in relatively short timescales (see Tenorio-Tagle \etal 1986 and
Franco \etal 1988). The cloud has been completely shocked at the time of the
second snapshot, and the lateral shocks have already disappeared. The cloud
mass is locked in the shocked layer and, due to its supersonic motion, a vacuum
is formed behind the layer. This rear vacuum
begins to be filled up by material falling from higher locations, as well as
from gas re-expanding from the shocked layer. This creates a pair of vortices,
one at each side of the layer, and a plume, or tail, is formed at the central
part of the rear wake. This is clearly seen in the third snapshot, at 9.5 Myr.
At this time, the shocked layer is already collecting gas from the denser parts
of the disk. The shock front decelerates as it penetrates into the disk, and
reaches the midplane at about 13 Myr. After crossing the midplane, the shock
accelerates in the decreasing density gradient, and blows out into the other
side of the halo. The beginning of the blow out process is apparent in the last
snapshot, at 19 Myr. The swirling motions of the rear wake, and the large
extent (about 1 kpc) and shape of the shocked layer inside the disk are clearly
displayed in this frame. A large fraction of the original cloud mass remains
locked up in the shocked layer, and a small amount of it has re-expanded back
into the rear wake and tail. In turn, the tail has expanded sideways and it has
a density minimum at the central part. This minimum is promoted by the
acceleration of the shock front after crossing the midplane. The size of the
perturbed region has grown close to 2 kpc in this last snapshot.

\subsubsection{HVC with $V_{HVC}$ = 200 km s$^{-1}$, and $\theta = 30^\circ$}

Figure 3 shows the hydrodynamical evolution for an oblique collision at $\theta
=30^\circ$. Again, the original cloud is located at 1250 pc from midplane, with
200 km s$^{-1}$, and the run is performed in the isothermal mode. Now the cloud
momentum has an important lateral component, which is conserved during the
evolution because the gravitational force has only a $z$-component. The first
two frames show the evolution of the shocked layer at 3.2 and 6.3 Myr,
respectively. The initial cloud is again completely shocked in a relatively
short timescale, before the first frame, and the vacuum left by the cloud
motion is filled up by infalling material and by re-expansion of the shocked
layer. The shapes of the interstellar structures are modified by the lateral
velocity component, but the main features of the hydrodynamical evolution are similar to the ones described in the previous case. The motion of the shocked
layer creates the rear wake (with vorticity and swirling motions), and a tail
that extends downstream to locations close to the point of impact.

The tail is now denser and more conspicuous than in the previous case, and it
has the appeareance of an elongated finger or cometary tail. There is a visible
shock in the second frame (at 6.3 Myr), when the central tail is forming. The
slower downward speeds, and the inclination of the structure, allows for the
gas of the tail to catch up with the main body of the shocked layer. The
velocity vectors within the structure are now larger, and clearly show the
re-expansion into the rarefied regions.  The shear between this faster flow and
its surrounding medium is subject to Kelvin-Helmholtz instabilities (\eg Shore
1992), but we cannot resolve the instability here. The oscillatory motion of
the finger-like tail, is due to the combined
effects of the vorticity of the rear flow and the unresolved instability. The
prominence of this tail structure increases with both increasing HVC velocities
and larger collision angles.

The main shock crosses the midplane at about 13 Myr, and accelerates
afterwards. As in the previous case, a density minimum is generated behind the
accelerated layer. Given that the acceleration is promoted by the density
gradient, is then directed along the $z$-axis and creates an elongation of the
structure in this direction. This is clearly apparent in the third frame, at
22.2 Myr. Again, the shock front begins to blow out of the disk at about these
times. The tail has also re-expanded at this time, and its vorticity and
oscillations have created a chaotic velocity field along the trajectory of the
interaction.

The late times evolution displays a wealth of features, illustrated in the last
snapshot at 47.7 Myr (to provide a better perspective, the midplane is now
located in the middle of the frame). The central parts of the disk are
distorted and compressed, with complex structures extending towards the impact
zone. The disk scaleheight is altered on both sides of the plane, and the
interphase between the upper and lower disk layers is marked but wavy, as in a
water-air interphase. At the incoming side, there are rounded tongues, and some
elongated structures breaking out from the disk, accompanied by a pair of
vortices above. At the other side, the blow out expansion is clearly apparent
and the front is reaching the lower edge of the grid.

\subsection{Magnetic disk with $B$ parallel to the $x$-axis: the role of
tension}

The rigidity and elasticity given to the disk by the magnetic field is better
accentuated in 2D when the plane of motion of the HVC is parallel to the field
lines, and the colliding gas distorts the initial field configuration. We
illustrate the response of these deformed field lines with three representative
cases. In these cases, the tension of the magnetic field dominates the
evolution, and the results are completely different from those of the purely
hydrodynamic cases. For the figures of these magnetic cases, where the
densities and velocities are indicated as before, the $B$-field lines are now
displayed with continuous lines.

\subsubsection{HVC with $V_{HVC}$ = 200 km s$^{-1}$, and $\theta = 0^\circ$}

The first MHD simulation is illustrated in Figure 4. It corresponds to a
collision perpendicular to the disk with cloud parameters identical to those of
Figure 2 (cloud located at 1250 pc, with velocity 200~km~s$^{-1}$ and impact
angle $\theta = 0^\circ$), except that the simulation is now performed in the
adiabatic mode.

The initial shock is strong and has a magnetic Mach number close to 4, with a
compression factor approaching 3 (a very strong shock has a compression factor
of 4, as in the non-magnetic case). With these parameters, there are thermal
shocks on both sides of the main shock front at the early evolutionary stages.
The lateral and downward shocks, however, disappear in relatively short timescales, and the MHD waves begin to move ahead of the shocked layer. The
first snapshot shows the expansion at $t$ = 3.2 Myr after impact. A series of
MHD waves are already driven in all directions, creating compressions and a
round shell-like structure (the ``bubble'') ahead of the shocked layer. The
lateral disturbances are Alfv\'en waves moving along the field lines, and the
disturbances in the $z$-direction are magnetosonic waves that compress the
field lines. The initial shock fronts (in either direction) move faster than
any of these waves, and are responsible for the strong deformation of the
initial field configuration but, as stated before, the key parameter
determining the outcome of this interaction is the downward distorsion of the
magnetic field.

During the first 7 Myr, a substantial fraction of the energy goes into the
compression and tension of the distorted field lines (the second frame shows
the evolution at 6.3 Myr).  Also, the disk material that is inside (and above)
the distorted sections slides down along the field lines, like in an inclined
plane, and settles down at the location of the magnetic valleys. Thus, the
distortions disrupt the local hydrostatic equilibrium, and there is a clear
infall of material in the perturbed region. This creates a dense ``head'' of
the perturbation moving towards the disk. The fast magnetosonic wave, moving in
the upper disk layers at an average speed of 50 km~s$^{-1}$, creates a strong
perturbation as it enters into the denser parts of the disk (it becomes a very
mild magnetic shock, that is apparent in the third frame, with a magnetic Mach
number always close to unity) and crosses the midplane at $t \sim 12$ Myr. At
about 8 Myr, the energy stored in the magnetic field begins to be released as
the field lines rebound, reversing the motion of the gas and lifting the dense
head (that has already penetrated a few hundred
pc into the lower layers) back to the upper parts of the disk. Thus, as seen in
the third and forth frames (9.5 and 15.9 Myr, respectively), a high-velocity
outflow moving away from the disk is created. This is a novel result in which
an incoming flow is forced to become an outflow by magnetic tension.

At about 13 Myr, and later on, the compressional and Alfv\'en waves carry most
of the available energy. The magnetosonic waves are able to perturb the other
side of the halo, and the Alfv\'en waves continue to drive the expanding
structure and create gas infall outside the location of the bubble. Thus, the
resulting structure is characterized by rising motions inside the bubble (from
the tensil restoring motion) and by lateral infall outside it.

Figure 5 shows a run with the same initial parameters of the previous model,
but now the evolution is isothermal. In this case, as expected, the shocked gas
piles up in a thin dense shocked layer that carries the momentum of the cloud.
Thus, now the compression and distortion of the field lines is more pronounced
in the zones where the momentum of the dense shocked layer is
concentrated, but the main evolutionary features are similar to the ones
described in the previous case. The evolutionary times shown in Figure 5 are
identical to those shown in Figure 4 (3.2, 6.3, 9.5, and 15.9 Myr). Comparison
with Figure 4 illustrates that the deformation of the field lines is now more
acute, leading to a sharp V-shaped form (almost a discontinuity) at 6.3 Myr. A
thin, dense, vertical structure is formed from the material that slides down
along the distorted field lines. The compressional wave also becomes a weak
MHD shock as it enters into the disk, and the lateral expansions, driven by Alfv\'en waves, are similar to the ones described in the previous case
(outflows in the central zones, and inflows in the external regions).

Except for differences in details and timescales, cases initiated at other $z$
locations and with different velocities behave in similar ways as the ones
described in Figures 4 and 5: the field prevents the penetration of the cloud
material into the disk and creates a net outflow at the late times evolution.
For instance, an isothermal case started at $ z =  350$ pc and with a speed of
100~km s$^{-1}$ encounters a rapid tensional rebound at about $t = 6$ Myr.

\subsubsection{HVC with $V_{HVC}$ = 200 km s$^{-1}$, and $\theta = 30^\circ$}

The oblique magnetic case is illustrated in Figure 6 by an isothermal collision
with $\theta = 30^\circ$ and 200 km s$^{-1}$, as in Figure 3. The galactic
shock has an important lateral component, producing a strong compression in the
$x$-direction, as seen in the first and second frames (3.2 and 6.3 Myr,
respectively). Once again, the magnetic field rebounds but the lines tend to
recover their original configuration in shorter timescales than in the
perpendicular cases. The motion of the shocked layer is again reversed as the
lines rebound (third frame at 15.9 Myr), and a series of prominent disk
oscillations and MHD waves are apparent during most of the evolution. The
horizontal component of the flow is maintained for a longer time (for instance,
it has a velocity of 47 km s$^{-1}$  at 20 Myr), and the patterns of the
velocity fields and magnetic field distortions are completely different to
those of the perpendicular cases.

As before, the Alfv\'en waves detach from the shocked layer, and create a
region with infalling gas that surrounds the shocked structure. The
magnetosonic waves also traverse the disk (becoming a weak MHD shock), and
perturb the other side of the halo. The tail is again formed behind the shocked
layer but the magnetic field now constraints the flows and
quenches the vorticity. The dense head moves almost parallel to the plane after
rebound. This creates a magnetic shear flow but the tension of the lines
prevents the appeareance of Kelvin-Helmholtz instabilities (\eg Frank \etal
1996; Malagoli \etal 1996; Jones \etal 1997).

The asymmetries in the distorted lines produce two important effects in the
tail. First, the downstream (right) field distortion has a larger extent, with
a softer slope, than the one created upstream (left). Thus, there is more mass
sliding down towards the tail from the downstream side. This provides
additional momentum to the tail, and creates a large rarified region behind it,
that is maintained for a long timescale (up to the end of the run). Second,
the gas that slides down from the upstream side provides an effective (ram
pressure) force that opposes to the motion of the tail. This is a
Rayleigh-Taylor unstable situation (\eg Shore 1992) but, as in the case of the
Kelvin-Helmholtz instabilities, we cannot resolve the instability. The undular
shape of the tail is long lived and is due to the unresolved instability. It
is still present at the fourth frame, at 41.2 Myr (also note that the shape of
the field lines are already distorted due to the Parker instability). In
summary, a complex network of asymmetrical features is
created, but the distorted tail moving almost parallel to the field lines is
the most prominent structure of the run.

Runs with other approaching angles and velocities generate the same type of
features, but with logical differences. As the incident angle is increased,
the asymmetries are increased: the
lateral component of the velocity is increased and the downward penetration is
reduced, but the lateral effects become more pronounced. The amplitude of the
maximum distortion in the field lines is reduced accordingly, and line
rebouncing occurs at earlier evolutionary times. For angles larger than
$\theta \sim 60^\circ$, the flow becomes
almost parallel to the $x$-direction. Nonetheless, the lines oscillate due to
the collision and the oscillations transmit MHD waves in all directions,
creating perturbations that are weaker but similar to those described before.

\subsection{Cases with $B$ perpendicular to the $x-z$ plane: the absence of
tension}

In theses cases, the magnetic field lines are oriented along the $y$-axis
(pointing outside of the figures). The lines preserve their straight alignment
in the $y$ direction as their footpoints are dragged along, in the $x-z$ plane,
by the flow motions. Thus, the lines are not distorted and there are no
Alfv\'en waves in these case. Also, there
are no tension effects, but the effects of magnetic pressure and field
compression are certainly present. Thus, the cloud gas can travel longer paths
and penetrate deeper into the disk. Also, the total pressure provides a very
effective drag that slows down the flow faster than in the purely
hydrodynamical case, and distorts the morphology of the shocked layer. The
evolution of these runs is intermediate to the previous non-magnetic and
magnetic-with-tension cases.

\subsubsection{HVC with $V_{HVC}$ = 200 km s$^{-1}$, and $\theta = 0^\circ$}

Figure 7 shows a model with the same cloud parameters as those of Figures 2 and
5 (isothermal evolution with 200 km s$^{-1}$ directed along the $z$-axis, and
the HVC is located at 1250 pc). The early times evolution resembles the one of
the purely hydrodynamical case described in section 4.1.1. The shocked layer
collects the gas and aquires a bow-shock form. The vacuum left behind the
shocked layer creates a swirling gas inflow, and a pair of vortices are
apparent behind the shocked layer during most of the simulation. As before, a
tail moving behind the shocked layer is created, and the differences with
the non-magnetic case begin to be
apparent when the decelerating shocked layer reaches the velocity of the
effective signal speed (at about 2 Myr). After this moment, the precursor
compressional perturbation begins to move ahead of the shocked layer (it is
already apparent, and located some 100 pc ahead of the shocked layer, in the
first frame at 3.2 Myr). As in the previous magnetic cases, the layer and its
precursor wave sink into the disk (second frame at 6.3 Myr), and the precursor
magnetosonic wave becomes a new magnetic shock wave that creates a second
shocked layer. Due to the lack of tension, the new MHD shock in this case is
stronger than in the previous magnetic cases (with a magnetic Mach number
ranging increasing from 1 to almost 3, as it penetrates into the central
regions).

The resulting new shocked layer collects only disk material, and is clearly
present in the third frame at 9.5 Myr. This shocked disk layer is the one
that actually penetrates into the central parts of the disk, and excites the
excites the magnetosonic perturbation that goes into the other side of
the halo (last frame at 19 Myr). The final fate of the first shocked layer, on
the other hand, which is the one that contains the gas from the impinging
cloud, is controlled by the magnetic pressure. The gas is forced to re-expand
by the compressed magnetic lines that have had accumulated in the space between
the two shocked layers, and it goes back to high $z$-locations. Again, then,
the cloud material cannot penetrate into the disk.

\subsubsection{HVC with $V_{HVC}$ = 200 km s$^{-1}$, and $\theta = 30^\circ$}

Figure 8 shows a model with $\theta = 30^\circ$ and the same parameters as in
Figures 4 and 6. The evolution follows the same basic features that were described in these previous models: a wake with swirling motions and a tail are
created behind the shocked layer, and a second shock front appears when the
compressional wave begins to penetrate the denser parts of the disk (first and
second frames at 3.2 and 9.5 Myr, respectively). Again, the structure and
evolution of the tail plays an important role in the evolution. The gas of the
tail catches up with the main body of the shocked layer, and a prominent and
elongated, finger-like, flow structure is created. As in the previous
non-magnetic case of Figure 4, the flow is subject to Kelvin-Helmholtz
instabilities, and the oscillatory motion of the structure (clearly apparent in
the third frame at 19 Myr) is due to vorticity and the unresolved
instability. Similarly, the prominence of the finger-like structure increases
with both increasing approaching velocities and larger collision angles.

In the case of the second shocked layer, there is one important difference with
respect to the previous perpendicular case: the two shocked layers are not aligned. The snapshot at 19 Myr shows that the new shock is directed along
the $z$-axis. This is due to the fact that the density gradient is directed
along this same axis. Thus, the second shocked layer moves perpendicular to the
plane of the disk, and the relative orientation between the two layers is
sensitive to the approaching angle of the cloud. The strength of this second
shock increases with increasing cloud velocities, but decreases with increasing
collision angles. Again, as in all previous magnetic cases, the cloud material
is unable to penetrate into the disk.

The late times evolution of the tail is almost identical to the one of the
non-magnetic case in Figure 3. The rounded (almost circular) tongues and
vortices extending along the trajectory toward the impact region (last frame
at 41.2 Myr), are long lived (up to the end of the run).

\section{Discussion and Conclusions}

We have presented simulations of HVCs collisions, at different incidence angles
and velocities, with magnetic and non-magnetic models of the Galactic thick
disk. In general terms, the structures formed in the non-magnetic cases are
similar to those discussed in previous studies, but some novel features are
uncovered here: the motion of the shocked layer creates a rear wake, with
vorticity, and a conspicuous tail. In oblique collisions, the tail becomes more
prominent and aquires an oscillatory motion that leads to a highly chaotic,
turbulent, velocity field along the trajectory of the interaction. Also, in
contrast with thin disk results, where the perturbed region has dimensions
similar to those of the original HVC, the resulting structures are larger and
better delineated.

The response of a magnetized thick disk, on the other hand, reveals new aspects
of the interaction. Such a disk, with a strong magnetic support at high-$z$,
also has important consequences for processes such as SN and superbubble
evolution (\eg Slavin \& Cox 1993; Tomisaka 1994, 1998). In contrast with
non-magnetic HVC-disk interactions, the cloud now encounters substantial
resistance through its evolution in the halo and cannot merge with the gaseous disk. The results with a magnetic field indicate that the perturbed volume is
certainly much larger than that of the non-magnetic counterparts. Moreover, if
the disk is Parker unstable, as it is the case of our warm
magnetic model, the collisions are able to excite different oscillation modes
in the disk and the halo, and do trigger the Parker instability (see Franco
\etal 1995 and Santill\'an \etal 1998). With a $B$-field in the $x$-direction,
the MHD waves propagate in all directions but any gas flow towards the disk is
drastically quenched. The tension effectively stops the shocked gas, and
reverses the motion of the flow, preventing any penetration of the original
HVC mass into the disk and creating gas motions, with velocities in the range
of 40 to 60 km s$^{-1}$, away from the disk. Thus, at least for this restricted
field geometry, the magnetic field represents an effective shield that prevents
any direct mass exchange between the halo and the disk.

For a $B$-field perpendicular to the plane of motion, the strength of the shock
also decreases rapidly but the compressional waves now have a more direct
effect on the central disk. The results for this field topology, which has
magnetic pressure but behaves in a tensionless manner, are intermediate to the
non-magnetic cases and the ones with magnetic tension. The shocked layer can
move deeper into the disk, but the buildup of magnetic pressure in the
compressed gas eventually stops the motion of the layer and forces its
re-expansion. The compressional waves, however, are transformed into a new
secondary shock front that penetrates into the disk. This creates a more
complex double shocked layer structure that lasts over several million of
years. The interaction of the new shock front with the inner disk layers alters
visibly the structure of the disk at large scales. Here again, however, the
cloud material cannot penetrate very deep into the disk.

The uniformity and symmetry of the disk and field modeled here are obvious
idealizations. At high $z$, a likely vertical component of the field should
modify the gas transport, and field line wandering would probably make the
fluid more viscous than modeled here. Thus, one might suspect that our results
would be altered in a 3D simulation. For instance, as suggested by the referee,
the field lines in the disk would split apart and let the cloud to go through
with much less resistance. Thus, our conclusions about bouncing clouds cannot
be conclusive and this issue requires a 3D verification. Due to the stochastic
nature of the Galactic magnetic field (Parker 1979), however, we anticipate
that some aspects of the behavior found in the two magnetic field topologies
considered here are bound to be present in more realistic 3-D cases. In
particular, it is hard to imagine a situation in which a cloud would not have
to fight magnetic tension from tangled and compressed field lines. Thus, at
least in some cases, a thick disk containing a bulky bundle of tangled lines could act as an effective shield against material penetration into the
innermost layers of the disk. Also, as stated before, the combined effects of
the Parker and magneto-rotational instabilities require three dimensional
studies with differential rotation. We are already making test runs with
additional field morphologies and, also, 3-D cases with a moderate resolution.
The results are encouraging, and a detailed analysis will be presented
elsewhere (Martos \etal 1999).

Summarizing, the magnetic field provides an adequate coupling for the energy
and momentum exchange between the disk and the halo, but inhibits the mass
exchange. The interactions can create strong MHD perturbations, with a
turbulent network of flows and vertical gas structures. Thus, the interstellar
$B$-field topology plays a paramount role in the final outcome of the
interaction with colliding clouds, and further studies with a magnetized disk will shed more light on the origin and fate of the HVC system.

\acknowledgments
We are grateful to Bruce Elemgreen, the referee, and Steve Shore, the editor,
for useful comments and suggestions. We also thank M. Norman, M. MacLow and R.
Fielder for continued consultory on Zeus. JF acknowledges useful, and heated,
discussions with Bob Benjamin and Bill Wall during the Interstellar
Turbulence conference, in Puebla, Mexico. AS thanks Victor Godoy and Juan
Lopez for their help with the visualization. This work has been partially
supported by DGAPA-UNAM grant IN130698, CONACyT grants 400354-5-4843E and
400354-5-0639PE, and by a R\&D grant from Cray Research Inc. The numerical
calculations were performed using UNAM's ORIGIN-2000 supercomputer.

\clearpage

redpajama_set_name: RedPajamaArXiv


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Points are accrued based on your choices and behaviors in the game. Attributes like making eye contact, sitting up straight, not fidgeting, are all things that can get you points. By the end of the game, you either land the job or you don't.
Unlike a real interview; however, by the time the decision is reached, you have learned the tricks of the trade. You walk away, no matter the decision, knowing where you messed up, where you should improve, how to think, how to behave in your next real-life interview.
First time interviewing? Or maybe you just want to brush up on your skills? JobPro games are available on the App Store, GooglePlay, and Amazon.
photo courtesy of sugar and spice ice cream
#SettingSail: Ice Cream Boat coming to Three Rivers
After waking up this morning to a layer of frost on my windshield, it's fair to say that the days of ice-scraping are creeping up quickly. With it we bid adieu to the flavorful ice cream season, but one local parlor has given Pittsburgh something to look forward to– a light at the end of the winter tunnel.
Spring of 2016 Sugar and Spice Ice Cream will christen its first ice cream boat to frequent the Pittsburgh's three rivers and deliver cold treats to customers on shore and on the water. That's right, an ice cream boat.
Sugar and Spice began as a traditional ice cream parlor. The family-owned business planted roots in Baldwin in 1984, but spread its wings to keep up with on-the-go customers.
Sugar and Spice took the wheel and embarked into the realm of Pittsburgh food trucks in August with the Sugar and Spice Ice Cream Truck. Out to tackle a new terrain, owners Lori and Kevin Heenan put down their ice cream scoops and picked up their hammers to remodel an old houseboat into an ice cream truck on water.
Jon Shanahan, Heenan's nephew and social media guru for the business, says the boat will match the truck in color– the same teal, pink and black scheme. If you know the truck, the boat will be easy to spot.
The Heenans hope to launch in April 2016, but stay up-to-date on construction through the boat's social media pages via Twitter and Facebook.
Don't quite have your sea legs? Never fear, the Sugar and Spice parlor and truck will remain open on land as well.
Photo by Laura Petrilla
#Wigle Whiskey: Finalist in Martha Stewart's American Made Contest
More potential recognition for Pittsburgh's Wigle Whiskey, which is a finalist in Martha Stewart's American Made Contest.
Wigle Whiskey made its name in Pittsburgh, for celebrating the city's expansive historical and cultural relationship to American whiskey. Wigle continues the region's tradition of quality whiskey using "a copper pot and local ingredients," according to the Wigle website.
The contest seeks out examples of what Pittsburgh does best: "the next generation of great American makers: Entrepreneurs, artisans and small-business owners who are creating beautiful, inspiring, useful products; pioneering new industries; improving local communities; and changing the way we eat, shop, work, and live."
The winner of the Martha Stewart American Made Contest will receive a trip to the Martha Stewart Living headquarters in New York City and $10,000. Only one winner will be selected.
The final results of online voting will be announced on Oct. 23.
This article appears in the October 2015 issue of The 412.
Categories: The 412
Pittsburgh Pet of the Week: Nellie
Why Learning CPR Can Help You Save a Life This Heart Month and Year-Round
Things To Do This Weekend in Pittsburgh

redpajama_set_name: RedPajamaCommonCrawl


text:
"""Tests for the PAM config checks."""

from grr.lib import flags
from grr.lib import test_lib
from grr.lib.checks import checks_test_lib
from grr.parsers import linux_pam_parser

class PamConfigTests(checks_test_lib.HostCheckTest):

  @classmethod
  def setUpClass(cls):
    cls.LoadCheck("pam.yaml")
    cls.parser = linux_pam_parser.PAMParser()

  def testPamSshAccess(self):
    """Test we handle when PAM ssh service doesn't require an account."""

    good1_contents = "account required pam_access.so\n"
    good2_contents = "account required /lib/security/pam_access.so foo\n"
    good3_contents = "account required /lib64/security/pam_access.so f b\n"
    bad_contents = "account required test.so\n"
    pam_good1 = {"/etc/pam.d/ssh": good1_contents}
    pam_good2 = {"/etc/pam.d/ssh": good2_contents}
    pam_good3 = {"/etc/pam.d/ssh": good3_contents}
    pam_bad = {"/etc/pam.d/ssh": bad_contents}
    sym = "Missing attribute: PAM ssh service must require an account."
    found = ["Expected state was not found"]
    results = self.RunChecks(
        self.GenFileData(
            "PamConfig", pam_bad, parser=self.parser))
    self.assertCheckDetectedAnom("PAM-SSH-PAMACCESS", results, sym, found)
    # Now the successful cases.
    results = self.RunChecks(
        self.GenFileData(
            "PamConfig", pam_good1, parser=self.parser))
    self.assertCheckUndetected("PAM-SSH-PAMACCESS", results)
    results = self.RunChecks(
        self.GenFileData(
            "PamConfig", pam_good2, parser=self.parser))
    self.assertCheckUndetected("PAM-SSH-PAMACCESS", results)
    results = self.RunChecks(
        self.GenFileData(
            "PamConfig", pam_good3, parser=self.parser))
    self.assertCheckUndetected("PAM-SSH-PAMACCESS", results)

  def testPamSshUnconditionalPermit(self):
    """Test we find when PAM ssh service allows an unconditional auth permit."""
    good_contents = "auth done pam_deny.so\n"
    bad_contents = "auth done pam_permit.so\n"
    pam_good = {"/etc/pam.d/ssh": good_contents}
    pam_bad = {"/etc/pam.d/ssh": bad_contents}
    # Check the detection case.
    sym = "Found: PAM ssh service has unconditional authentication."
    found = ["In service 'ssh': auth done pam_permit.so"]
    results = self.RunChecks(
        self.GenFileData(
            "PamConfig", pam_bad, parser=self.parser))
    self.assertCheckDetectedAnom("PAM-SSH-UNCONDITIONAL-PERMIT", results, sym,
                                 found)
    # Now the pass case.
    results = self.RunChecks(
        self.GenFileData(
            "PamConfig", pam_good, parser=self.parser))
    self.assertCheckUndetected("PAM-SSH-UNCONDITIONAL-PERMIT", results)

  def testPamSshDefaultDeniesAuth(self):
    """Test we detect when PAM ssh service doesn't deny auth by default."""
    good1_contents = "auth required pam_deny.so\n"
    good2_contents = ("auth [success=ok new_authtok_reqd=ok default=die] "
                      "pam_unix.so try_first_pass\n")
    bad_contents = "auth required pam_foobar.so\n"
    pam_good1 = {"/etc/pam.d/ssh": good1_contents}
    pam_good2 = {"/etc/pam.d/ssh": good2_contents}
    pam_bad = {"/etc/pam.d/ssh": bad_contents}
    # Check the detection case.
    sym = "Missing attribute: PAM ssh service must default to denying auth."
    found = ["Expected state was not found"]
    results = self.RunChecks(
        self.GenFileData(
            "PamConfig", pam_bad, parser=self.parser))
    self.assertCheckDetectedAnom("PAM-SSH-DEFAULT-DENIES-AUTH", results, sym,
                                 found)
    # Now the pass cases.
    results = self.RunChecks(
        self.GenFileData(
            "PamConfig", pam_good1, parser=self.parser))
    self.assertCheckUndetected("PAM-SSH-DEFAULT-DENIES-AUTH", results)
    results = self.RunChecks(
        self.GenFileData(
            "PamConfig", pam_good2, parser=self.parser))
    self.assertCheckUndetected("PAM-SSH-DEFAULT-DENIES-AUTH", results)

  def testPamSshNoNullPasswords(self):
    """Test we find when PAM ssh service allows an unconditional auth permit."""
    good_contents = "password sufficient pam_unix.so\n"
    bad_contents = "password requisite /lib/security/pam_unix.so nullok\n"
    pam_good = {"/etc/pam.d/ssh": good_contents}
    pam_bad = {"/etc/pam.d/ssh": bad_contents}
    # Check the detection case.
    sym = "Found: PAM ssh service allows unix null password accounts to login."
    found = [
        "In service 'ssh': password requisite /lib/security/pam_unix.so "
        "nullok"
    ]
    results = self.RunChecks(
        self.GenFileData(
            "PamConfig", pam_bad, parser=self.parser))
    self.assertCheckDetectedAnom("PAM-SSH-NO-NULL-PASSWORDS", results, sym,
                                 found)
    # Now the pass case.
    results = self.RunChecks(
        self.GenFileData(
            "PamConfig", pam_good, parser=self.parser))
    self.assertCheckUndetected("PAM-SSH-NO-NULL-PASSWORDS", results)

  def testPamSecureDefaults(self):
    """Test we detect when PAM ssh service doesn't deny auth by default."""
    good_contents = """
        auth required pam_deny.so foobar
        password sufficient /lib64/security/pam_warn.so
        session requisite /lib/security/pam_deny.so
        """
    bad_contents = good_contents + """
        auth required pam_permit.so
        password done pam_foobar.so test args
        """
    pam_good = {"/etc/pam.d/other": good_contents}
    pam_bad = {"/etc/pam.d/other": bad_contents}
    # Check the detection case.
    sym = ("Found: PAM 'other'(the default) config should only be "
           "used for denying/logging access.")
    found = [
        "In service 'other': auth required pam_permit.so",
        "In service 'other': password done pam_foobar.so test args"
    ]
    results = self.RunChecks(
        self.GenFileData(
            "PamConfig", pam_bad, parser=self.parser))
    self.assertCheckDetectedAnom("PAM-SECURE-DEFAULTS", results, sym, found)
    # Now the pass cases.
    results = self.RunChecks(
        self.GenFileData(
            "PamConfig", pam_good, parser=self.parser))
    self.assertCheckUndetected("PAM-SECURE-DEFAULTS", results)

  def testPamExternalConfigs(self):
    """Test we detect when PAM ssh service doesn't deny auth by default."""
    pam_good = {
        "/etc/pam.d/ssh": "auth include other",
        "/etc/pam.d/other": ""
    }
    pam_bad = {
        "/etc/pam.d/ssh": "auth include non-existant",
        "/etc/pam.d/other": "password include /tmp/non-existant"
    }
    # Check the detection case.
    sym = "Found: PAM configuration refers to files outside of /etc/pam.d."
    found = [
        "/etc/pam.d/ssh -> /etc/pam.d/non-existant",
        "/etc/pam.d/other -> /tmp/non-existant"
    ]
    results = self.RunChecks(
        self.GenFileData(
            "PamConfig", pam_bad, parser=self.parser))
    self.assertCheckDetectedAnom("PAM-EXTERNAL-CONFIG", results, sym, found)
    # Now the pass cases.
    results = self.RunChecks(
        self.GenFileData(
            "PamConfig", pam_good, parser=self.parser))
    self.assertCheckUndetected("PAM-SECURE-DEFAULTS", results)

  def testPamConfigPermissions(self):
    """Ensure check detects Pam config files that non-root users can edit."""

    data = [
        self.CreateStat("/etc/pam.d/hit-123", 50, 0, 0o0100640),
        self.CreateStat("/etc/pam.d/hit-234", 0, 60, 0o0040777),
        self.CreateStat("/etc/pam.d/no-hit-123", 0, 6000, 0o0100440),
        self.CreateStat("/etc/pam.d/no-hit-234", 0, 0, 0o0100640),
        self.CreateStat("/etc/pam.d/hit-345", 70, 0, 0o0100660)
    ]

    results = self.GenResults(["LinuxPamConfigs"], [data])

    check_id = "PAM-CONFIG-FILES-WRITABLE-BY-NON-ROOT-USER"
    sym = ("Found: Files or folders in Pam configuration can be modified by "
           "non-privileged users.")
    found = [
        "/etc/pam.d/hit-123 user: 50, group: 0, mode: -rw-r-----",
        "/etc/pam.d/hit-234 user: 0, group: 60, mode: drwxrwxrwx",
        "/etc/pam.d/hit-345 user: 70, group: 0, mode: -rw-rw----",
    ]

    self.assertCheckDetectedAnom(check_id, results, sym, found)

def main(argv):
  test_lib.GrrTestProgram(argv=argv)

if __name__ == "__main__":
  flags.StartMain(main)

redpajama_set_name: RedPajamaGithub


Since joining The Stogsdill Law Firm, P.C. in 2006, Mr. Williamson has worked exclusively in the field of matrimonial law. Mr. Williamson is dedicated to providing his clients, no matter the issue, with the experience and knowledge necessary to bring their case to a positive resolution. Mr. Williamson has successfully negotiated settlements and/or litigated issues involving complex financial matters, custody, support and division of property. Mr. Williamson has also successfully negotiated custody/financial settlements as they relate to paternity actions.
Mr. Williamson is also the general counsel and associate board president of Griffith Tutoring. Griffith Tutoring is a non-profit organization preparing at-risk Chicago high school students for the ACT college entrance exam by partnering with businesses and training their professionals to tutor and mentor the students.
Mr. Williamson received a Juris Doctorate degree from The John Marshall Law School in December 2005. Mr. Williamson completed his undergraduate studies at Butler University, where he graduated with a BA in History and English, and also received honors from the History department.
While at Butler, Mr. Williamson was also a member of the Division 1 Lacrosse Team and the Sigma Chi fraternity. Prior to joining The Stogsdill Law Firm, P.C., Mr. Williamson worked as an insurance coverage associate attorney at Bollinger, Ruberry & Garvey in Chicago, Illinois. Mr. Williamson's previous position provided him with a wealth of knowledge and experience in researching and resolving a wide array of contractual issues.
Mr. Williamson is a member in good standing of the DuPage County, Will County, Chicago, and Illinois Bar Associations. Mr. Williamson is involved in the DCBA mentor-mentee program serving as a mentor to a newly admitted member of the Illinois State Bar. Mr. Williamson has been appointed to the Hearing Board of the Attorney Registration and Disciplinary Commission (ARDC) where he sits on a 3 Judge Panel ruling upon violations of attorneys of the Rules of Professional Conduct.


text:
moon-rock-server
================

An experimental server for working with recorded space walk sessions


It has a hardness of about 6 on the Mohs hardness scale. It is one of two minerals in ... Milky quartz is a common mineral that is found in many different types of rocks.
Start studying Chapter 17. Learn ... Which type of rock probably ... The property that is not considered useful in identifying minerals is Answer a. hardness.
Mohs' original hardness values are highlighted in yellow. The selection of mineral species for hardness standards is based on the common availability of the mineral.
There are many types of rocks and minerals, but do you know how to distinguish one from another? On this page you will learn about things like lustre and the Mohs hardness scale, to sedimentary and igneous rocks.
... and metamorphic rock types with this handy rock identification ... rock's grain size and hardness. ... and refers to the minerals contained within a rock.
Rock Physical Property Tests Rocks are made of one or ... rocks because each type of rock has a different ... can be used to determine mineral hardness.
Mineral Hardness . The hardness of a mineral is a way of describing how easy or difficult it is to scratch the mineral. It is used, in combination with the other physical properties, to help identify a mineral specimen.
Suggested Methods for Determining Hardness and Abrasiveness of Rocks ... on the type and quantity of the various mineral con- ... vidual rock minerals.
Chapter 4 Rocks and Minerals. Chapter 4 focuses on Rocks and Minerals, looking at types of rocks. ... are used to determine the relative hardness of a rock or mineral.
... learn different types of rocks, and how rocks and minerals are used in everyday items. ... or hardness. -Minerals can be rocks, and rocks are made of minerals.


text:
360daily
360daily Features
iOS 11 & 10.5 Inch iPad Pro Unveiled, OnePlus Support, Nubia Z17 mini Launch, and More: Your 360 Daily
iOS 11 & 10.5-Inch iPad Pro Unveiled, OnePlus Support, Nubia Z17 mini Launch, and More: Your 360 Daily
By Gadgets 360 Staff | Updated: 6 June 2017 23:17 IST
You could pay for UPI transactions from June 10
Apple could bring jobs to India in exchange for tax breaks
Nintendo reveal three Pokemon games and their release dates
At WWDC 2017, Apple showed off a revamped iOS 11 along with changes to the App Store. Support for 32-bit apps will end when iOS 11 hits, and even macOS High Sierra - Apple's next desktop OS, will drop support for 32-bit apps. The new software for iPhone and iPads will bring faster Safari browser, smarter Siri, redesigned Control Centre, Files app, and several other new features. At the event, Apple also unveiled a new 10.5-inch iPad Pro model with thinner bezels, better screen, cameras the same as iPhone 7's, along with a refreshed 12.9-inch iPad Pro; the two models will be launched in India next month. The MacBook lineup also got a refresh as did a new iMac, while an all-new iMac Pro was unveiled, with release scheduled for December.
In other Apple news, albeit closer to home, India wants Apple to create jobs in exchange for tax benefits. The move comes amid concerns that growth in Asia's third-largest economy isn't helping add jobs.
OnePlus claims improved customer support in lead up to OnePlus 5 launch
In the lead-up to the launch of its OnePlus 5 flagship smartphone, the company has now released a video to showcase the improved customer service support that will now be available to its users. The company says that from five people initially in customer service, it now has around 500 people in the customer support department. It says that it now has customer service centres in 10 different locations around the world. OnePlus says that users simply need to contact the company, by either calling, through live chat or social media, or by one of its forums and it will then take care of pickup, transport, as well as repair and returns.
UPI payments may become chargeable soon
The Unified Payments Interface (UPI) is the Indian government's attempt to convert the masses to cashless payments. The intent was to allow money transfer between two bank accounts with a phone. Many banks followed the governments regulation and launched their own UPI apps. After a holiday period UPI transactions will be chargeable from July 10 onwards.
As per an email sent by HDFC bank to some customers, it informs its customers that "all UPI outward transactions will be chargeable from 10th July 2017". For transaction amount of Re. 1 to Rs. 25,000, the fee will be Rs. 3 plus taxes, and for transaction amount of Rs. 25,001 to Rs. 100,000, the fee will be Rs. 5 plus taxes. This email was first shared on Reddit by a user named Gatiman.
Nubia Z17 mini with dual rear cameras launched in India
ZTE sub-brand Nubia has launched the Z17 mini smartphone with dual rear cameras (13-megapixels monochrome + RGB) in the Indian market at Rs. 19,999 in exclusive partnership with Amazon. The smartphone has a 5.2-inch full-HD screen with nearly no bezels on the sides, and runs Android Marshmallow software. Other key Nubia Z17 mini specifications include octa-core Snapdragon 652 processor, 4GB RAM, 64GB internal storage, up to 200GB microSD card support, and 2950mAh battery.
Huawei Honor 9 release date; Honor 6X price drop
The Honor 9 smartphone, which has earlier been a part of leaks, has now received an official launch date. In line with a poster leaked last week, the new official poster has confirmed that Honor 9 will be launched by the company at its June 12 event. The launch poster teases the dual camera setup on the smartphone just like the previous leaks. To recall, the Huawei Honor 9 is expected to feature a 20-megapixel + 12-megapixel sensor at the back of the smartphone, as per the report. The phone has further been tipped to be powered by a HiSilicon Kirin 960 SoC coupled with either 4GB or 6GB of RAM.
In other Honor news, Huawei has decided to slash the price of the Honor 6X smartphone in the country. The Honor 6X is now available to purchase from Amazon India exclusively, at a price starting at Rs. 11,999. The Honor 6X was launched at Rs. 12,999 and Rs. 15,999 for the 32GB and 64GB variant exclusively. However, the price has now been reduced to Rs. 11,999 and Rs. 13,999 respectively. The smartphone is exclusively available on Amazon India for purchase, and the new prices are already reflecting on the e-commerce site.
Android June Security Update rolling out to Nexus and Pixel owners, fixes Pixel freezing issue
Google is now rolling out the Android June security update for Pixel and Nexus users. This update brings a number of bug fixes and security patches, the most notable one being a fix for Pixel users experiencing the sporadic freezing issue since sometime. Factory and OTA images are already live for compatible devices. This update can be downloaded for Google Pixel, Pixel XL, Pixel C, Nexus 6P, Nexus 5X, Nexus Player, Nexus 6, and Nexus 9 devices. On the Google Product forum, an employee has confirmed that the patch also brings a fix for the Pixel freezing issue.
Siri, WeChat, and other apps may put you at risk of voice hacking: study
Siri, WeChat and other voice-based smartphone apps can expose you to voice hacking, warn scientists who are developing a new app to stop the growing security threat.With just a few minutes of audio samples, attackers can replay your voice convincingly enough to trick people as well as top digital security systems, researchers said.
The consequences, from impersonating you with your friends to dipping into your bank account, are terrifying, they said. Using only tools already on smartphones, a team of engineers led by University at Buffalo in the US is creating an app to stop voice hacking.
Yu Yureka Black goes on sale in India via Flipkart
The Yu Yureka Black has gone on sale in India via Flipkart from Tuesday. The Yureka Black is the latest offering from Micromax's Yu Televentures, the first smartphone from its stables in more than six months.
The smartphone was launched in Chrome Black and Matte Black colour variants. The Yu Yureka Black price in India is Rs. 8,999, and it competes with the Xiaomi Redmi 4 and Coolpad Note 3 Lite.
Though it runs the dated Android 6.0 Marshmallow, the Yu Yureka Black packs a few software features. These include an ability to easily take and save screenshots by sliding three fingers; a one-handed-mode; ability to take full page screenshots; double tap screen to unlock device; and double tap home button to lock the phone. You can also flip the Yu Yureka Black to mute it when you are getting an incoming call; lift phone to call a contact, and flip the phone to snooze an alarm.
Lenovo unveils range of Think desktops, laptops, and monitors in India
Lenovo has launched in India the 2017 range of ThinkPads, ThinkCentres and Tiny-in-Ones (TIOs) that are powered by 7th Generation Intel Core i7 processors. The new Lenovo products include ThinkPad X1 Carbon, ThinkPad X1 Yoga, ThinkPad X270, ThinkPad Yoga 370, ThinkPad L470, ThinkPad T470, ThinkPad T470s, and ThinkCentre M710 Tiny Desktop, among others.
ZTE V870 with 4GB RAM, Snapdragon 435 SoC launched
ZTE has launched the all-new V870 mid-range smartphone in its homeland. Priced at CNY 2,699 (roughly Rs. 25,500), the ZTE V870 smartphone is now available to buy in China. The new ZTE V870 sports an all-metal body, and features a fingerprint scanner at the back. The device also sports dual speakers at the bottom panel.
For specifications, ZTE V870 features a 5.5-inch full-HD IPS display. It is powered by an octa-core Qualcomm Snapdragon 435 processor clocked at 1.4GHz coupled with 4GB of RAM. It packs 64GB inbuilt storage, and supports expandable storage via microSD card (up to 128GB). On the camera front, it sports a 16-megapixel rear camera with LED flash and f/2.0 aperture. There's also an 8-megapixel front camera on-board. The phone ships with a 3000mAh non-removable battery. The V870 runs on Android 7.0 Nougat and support 4G connectivity apart from other standard connectivity options. It measures 156x76x7.8mm.
Pokemon Direct: Pokken Tournament DX, Pokemon Ultra Sun and Ultra Moon announced
Nintendo announced fighting game Pokken Tournament DX for the Nintendo Switch. It's a fighting game featuring Pokemon. It will be available from September 22. Also revealed was Pokemon Ultra Sun and Ultra Moon for the Nintendo 3DS with a November 17 release date. These are enhanced versions of 2016's Pokemon Sun and Moon. And there's more, GameBoy Color classics, Pokemon Gold and Silver also see a re-release on the Nintendo 3DS Virtual Console on September 22.
Further reading: 360 daily, Pokemon, Android, Apple, iOS 11, WWDC 2017, UPI, Honor 9, Honor 6x, Yu Yureka Black, Siri, WeChat, Voice Hack, ZTE v870, OnePlus 5, Lenovo, Lenovo Thinkpad, Pokken Tournament DX, Pokemon Ultra Sun and Ultra Moon
Gadgets 360 Staff Email Staff The resident bot. If you email me, a human will respond. More
Pokemon Direct 2017: Every Pokemon Game and Release Date for Nintendo Switch and 3DS You Need to Know
India Price of New iPad and Mac Models Apple Announced at WWDC 2017
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360 Daily
Asus Zenfone AR India Launch, Jio Effect, Moto E4 Plus Sale, and More: Your 360 Daily
Nokia 3, 5, 6 India Launch Date, Moto C Comes to India, and OnePlus 5 Design: Your 360 Daily
Vivo V5s Launched, Moto E4 Leaked, iPhone 8 Rumours, and More: Your 360 Daily
Super Mario Run Launch, Yahoo's 1 Billion User Hack, and More: Your 360 Daily
Mirzapur Season 2 First Look Reveals Amazon Series to Return in 2020
MESSAGE Gadgets 360 Staff


Glendale Educational-Community Scholarship ($500.00) – randomly drawn from a list of select student candidates who have earned a minimum 90% GPA, have completed the 'student scholarship information form' and have been accepted to an institute of higher education.
The Glendale School District Education Foundation, in cooperation with the Glendale High School guidance and administrative offices, would like to invite/request more local businesses, organizations, alumni and individuals to please consider sponsoring scholarships for our Glendale High School graduating seniors. While the students at our small rural school district are prepared academically for college and/or other institutes of higher learning, there endures a significant lack of scholarship monies. Glendale graduates seeking to attend institutes of higher learning need your help--especially in light of the fact that we have lost well over seven scholarship sponsors the past few years! Whether you are former alumni, local business owner or civic organization leader, we strongly encourage you to please give back to the children of your alma mater by providing funding for our high school graduates for annual gifts as little as $250--which (should you choose) could be distributed through our non-profit 501(c)(3) Foundation.
Scholarships could be placed in the name of organizations, memorials for loved ones, or to honor former teachers, coaches, or individuals. These awards are handed out annually in May to our Glendale High School seniors. What better way to 'invest in our community's future' than through our students?
Interested in giving back to the graduating seniors at Glendale? Contact the Glendale Education Foundation executive director, Richard W. Snyder II, via phone (814) 312-8620 or email: rsnyder@gsd1.org Mr. Snyder looks forward to hearing from you and is available to assist in any way--with a special expertise in helping design the criteria of your annual scholarship.


text:
STUDY FINDS 'NO-BRAINER' HEDGE
Susan Barreto
NEW YORK -- Plan sponsors are starting to take inflation-indexed bonds seriously, said Christopher K. Kinney, manager at Brown Brothers Harriman & Co.
Brown Brothers, in conjunction with BARRA RogersCasey, Berkeley, Calif., completed research detailing asset mixes of individual defined contribution plan participants with the incorporation of Treasury inflation-indexed securities. It is the first study of its kind, according the firm.
Inflation-indexed bonds are a good inflation hedge with a low correlation to other asset classes and are viable investments for defined benefit plans, defined contribution plans and foundations. "It's a no-brainer," Mr. Kinney added.
He suggests an allocation of 10% of total assets for pension funds and the full 25% of the assets in defined contribution plans estimated to be in guaranteed investment contracts, stable value funds and money markets.
Inflation itself has had a correlation of -0.28 with stocks, 0.05 to intermediate Treasury bonds and 0.69 with T-bills in the past 50 years. The study also says nominal return vs. real return for intermediate government bonds for the past 50 years, on an annualized basis, was 6.04% vs. 2.02%, thanks to inflation.
There always will be the need for conventional bonds in a portfolio to offset the risk of deflation, said Mr. Kinney. "But if one were ambivalent whether inflation will go up or down, then a strong argument will be made to allow inflation-indexed securities to supplant the conventional bond."
Brown Brothers Harriman manages a small amount of inflation-indexed securities in its separate accounts when it is feasible, in addition to its mutual fund, 59 Wall Street Inflation Index Securities Fund, which has $13 million.
Other companies that have inflation-indexed Treasury mutual funds are Pacific Investment Management Co., Newport Beach, Calif.; American Century, Kansas City, Mo.; and Teachers Insurance Annuity Association-College Retirement Equities Fund, New York.
According to the research, individual investors can handle inflation rates of 10% before the real return becomes negative in a tax-deferred portfolio.
The authors analyzed differing allocations to the Treasury inflation-indexed securities by the age of the investor when he or she starts saving and expected retirement age. The result: The earlier the saving begins, the earlier the inflation-indexed Treasury allocation should begin to ensure an early retirement.
The model in the research used the returns of the Standard & Poor's 500 stock index and 30-day Treasuries from 1953 to the present.
An asset allocation of 80% stocks and 20% inflation-indexed Treasuries, until age 60 or so, is the mix suggested by the Brown Brothers and BARRA research. At retirement at age 65, the mix is 40% stocks and 60% inflation-indexed Treasuries.
William Lloyd and Henry Willmore at Barclays Capital, New York, see the 30-year inflation-linked bonds as "an attractive investment opportunity." Mr. Willmore, a senior economist at the investment banking firm, and Mr. Lloyd, head of marketing strategy, are predicting the core inflation rate will increase to 2.8% from 2.5% in the second half of the year and to more than 3% in 1999.
Barclays currently trades about 18% of the total inflation indexed market.
Consultants have yet to embrace the concept.
Warren Mulhern, director of operations for Advest Custom Consulting, Hartford, Conn., said his firm concluded the bonds were a great idea, but with the current environment of nonexistent inflation, it's hard to convince clients to add them as an asset class.
"In the late '70s when we had double-digit inflation, it would have been like a cure for cancer," Mr. Mulhern said.
But Jeffrey Ross, a consultant with Arnerich & Massena, Seattle, said he doesn't see any advantages.
Clients of Buck Consultants have not shown interest in using the bonds either, said Jonathon Mueho, investment consultant.
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