A&A 412, 745-749 (2003)
DOI: 10.1051/0004-6361:20031477
A. C. Raga1 - J. Cantó2
1 - Instituto de Ciencias Nucleares, UNAM, Ap. 70-543,
04510 D F, México
2 -
Instituto de Astronomía, UNAM, Ap. 70-264,
04510 D F, México
Received 19 May 2003 / Accepted 4 September 2003
Abstract
We propose that some low excitation HH objects might
correspond to the head of a pulsed jet moving into a dense environment.
We develop an analytic model showing that the head of such a jet
will move slowly, producing a low excitation bow shock. At the
times at which the successive pulses catch up with the jet head,
high excitation emission will be produced, lasting for a time
of the order of the cooling timescale of the material heated
in the pulse/jet head interaction. In this way, the jet head
has "flashes'' of high excitation emission superimposed
on a "quiescent'', low excitation emission.
Key words: ISM: Herbig-Haro objects - ISM: jets and outflows - ISM: kinematics and dynamics - shock waves
The spectra of HH objects appear to fall in two more or less well defined categories: "low excitation spectra'' (with strong lines of neutrals and some singly ionised species) and "high excitation spectra'' (with strong lines of singly and twice ionised species). An attempt to quantify these two spectral categories can be found in Raga et al. (1996).
A well studied (but not fully understood) effect is that the knots along
a HH jet have low excitation
spectra implying shock velocities of
km s-1,
which are considerably lower than the
km s-1measured jet velocities. Three different possibilities have been proposed
in order to explain this effect:
It is of course less clear how to obtain low excitation emission
in the leading head of an HH jet. In the head of a jet, the jet
velocity is split between the bow shock and the Mach disk (or "jet shock'').
Therefore the head of a 300 km s-1 jet will have one shock with
a shock velocity
km s-1 and a second
shock with
km s-1 (whether the bow shock or the
Mach disk is the faster shock being decided by the jet-to-ambient
density ratio, see Hartigan 1989; Raga & Noriega-Crespo 1993) and
should therefore have a high excitation spectrum.
A possibility for explaining an observed low excitation "head'' is to have a significant velocity decrease along the beam of the jet (which could be the result of a "slow startup'' of the ejection or more likely a result of the interaction with the surrounding environment). In this way one has a fast flow close to the source (as observed) and a slower flow immediately upstream of the head of the jet. This possibility has been explored in the context of the HH 34 giant jet by Cabrit & Raga (2000), de Gouveia Dal Pino (2001) and Masciadri et al. (2002). It is not clear, however, whether such models could explain the low excitation heads of "shorter'' flows such as HH 7-11 (see, e.g., Noriega-Crespo & Garnavich 2001).
In the present paper we propose the following, alternative model. A jet with a variable ejection velocity generates a series of "internal working surfaces'' which contain most of the material of the outflow (see, Raga & Kofman 1992; Cantó et al. 2000). These internal working surfaces move at a velocity v0 which is determined by the mass and momentum contained in each "ejection event'' or "pulse'' of the time-dependent ejection (this velocity does not depend on the properties of the surrounding environment, as the working surfaces travel into the "channel'' which is left behind by the passage of the head of the jet). If the jet travels into a dense enough environment, the head of the jet will move at a low velocity, and will be impacted upon by the successive "clumps'' (i.e., the internal working surfaces) which catch up with the jet head.
In this flow configuration, the head of the jet has a low velocity bow shock, and therefore produces a low excitation spectrum. As the jet beam is composed of "clumps'' (rather than being a continuous flow), the head has no Mach disk, except at the times at which the clumps impact on the head. Therefore, the high excitation spectrum of the Mach disk is absent at most times. In this way, a variable jet moving into a high density environment will produce a slow moving head, which most of the time emits a low excitation spectrum, and emits a high excitation spectrum only in "flashes'' corresponding to the times in which the successive internal working surfaces catch up with the jet head.
In Sect. 2, we present a simple, analytic model (based on mass and momentum conservation considerations) describing the motion of the head of the jet. The emission properties of the jet head are described in Sect. 3. Finally, the results, implications and limitations of the model are discussed in Sect. 4.
In order to derive the equation of motion for the head of a variable jet we consider the situation shown in the schematic diagram of Fig. 1. We assume that the jet beam is formed by a series of "clumps'', which travel away from the source at a velocity v0. These clumps could be directly associated with the form of the time-dependent ejection, or alternatively could be the result of an abritrary ejection velocity variability which then leads to the formation of internal working surfaces which contain most of the mass and momentum of the jet beam (see Raga & Kofman 1992; Cantó et al. 2000).
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Figure 1:
Schematic diagram showing the structure of a pulsed
HH jet. The "internal working surfaces'' are idealized as clumps
travelling at a (constant) velocity v0. The head of the
jet (at position ![]() ![]() |
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Due to its direct interaction with the environment, the head of
the jet moves with a velocity
.
Therefore the "clumps''
along the jet beam catch up with the head, supplying it with more
mass and momentum.
![]() |
Figure 2:
Diagram showing the position ![]() ![]() ![]() ![]() ![]() |
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Figure 2 shows the situation found for a periodic ejection variability
with pulses of mass M0 and velocity v0 ejected with a period .
The first "clump'' is ejected at t1=0, and starts interacting
with the environment at x1=0 (where the x-coordinate corresponds
to the distance from the source along the outflow axis, see Fig. 1).
The following clumps are ejected from the source at times
,
,
,
etc., and are assumed to
travel unimpeded at a velocity v0 until they catch up with
the head of the jet. We assume that these clumps do not expand
sideways beyond the "channel'' left behind by the jet head, which
is probably reasonable given the very high Mach
numbers (of
)
estimated for HH jets. The trajectories
of these clumps in the (x,t) plane are depicted by the dashed lines
in Fig. 2. The successive clumps catch up with the jet head at
positions and times (x2,t2), (x3,t3), etc. (see Fig. 2).
Depending on the parameters of the flow, one could have situations
in which the successive clumps do not travel into an "empty
channel'' and could be dynamically affected by their interaction
with the material filling up the interclump region. For this to
take place, the gas in the "cocoon'' surrounding the jet beam (which is
composed of shocked environmental material and jet material ejected
sideways by the jet head) has to be able to fill
in the channel in the period
between the passage of two
successive knots. The condition for the channel to be filled in
is therefore
Let us now derive the equation of motion for the position
of the
head of the jet (see Fig. 2) for the segment of its trajectory between
the points (xn,tn) and
(xn+1,tn+1). If we assume
that the jet has a position-independent radius rj, and that the head
of the jet has all of the mass of the "clumps'' that have reached
it as well as the mass of the swept-up environment, the mass of the
head is then given by:
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Figure 3:
Solutions for the position
![]() ![]() ![]() ![]() ![]() |
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We can also see from Fig. 3 that while the position of the jet head is (as hoped) continuous as a function of time,
its velocity
is not, as it has discontinuous jumps
at the times at which the clumps catch up with the jet head.
By combining Eqs. (10) and (12) we can
obtain the velocities immediately to the left
The continuous segments of the
vs. t dependence of the
motion of the head of the jet (see Fig. 3) emit energy in a continuous
way as a function of time. Considering that for a high Mach number,
highly radiative flow the thermal energy is negligible, then the rate
of change of the kinetic energy of the head of the jet (in the continuous
segments, in which no new kinetic energy is being injected into the head)
has to be equal to the radiative luminosity of the flow:
When the successive clumps catch up with the head of the jet,
we have a "discrete'' amount of energy which is emitted as
a result of the interaction process. This energy can be computed
in a straightforward way as the difference between the
clump+head kinetic energy (just before the interaction),
and the kinetic energy of the "merged''
clump+head:
Of course, this energy is not ejected at a single instant (as
implied by our simplified analytic model), but extends over
a time
which depends on the size of the clumps along
the symmetry axis (which has been implicitly set to zero in
Sect. 2) and on the cooling timescale of the gas heated in the
collision of the clump with the jet head.
If the emission due to the clump/head collision "flashes'' lasts
for a time
,
the resulting luminositiy would
be given by
![]() |
Figure 4:
Total luminosity of the jet head (in units
of
![]() ![]() ![]() ![]() |
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In Fig. 4, we show the total luminosity
(see Eqs. (16) and (19)) as a function of time for a model with
and different values of
.
For this
value of
,
the "flashes'' (resulting from the clump/jet
head catching up processes) last for 10% of the time, and
have luminosities which are 1.5 to 2 orders of magnitude higher
than the luminosities of the "quiescent'' periods between the
flashes.
In the "small '' regime (i.e., in which the interaction+cooling
time
is shorter than the period of the ejection variability), we then
have short "flashes'' separated by long quiescent periods. In models
with low
,
the velocity
of the
jet head will be substantially lower than the jet velocity v0 (see
Eqs. (12) and (15)). Therefore, in the quiescent periods (when
the emission comes from the bow shock which has a shock velocity equal
to
)
will have a low excitation spectrum.
In the "flashes'', we will see the emission of a shock of velocity
(which is comparable to v0 in the
regime)
lasting for the duration time of the clump/jet head collision.
As the clumps along HH jets do not show
large extensions along the outflow axis,
the interaction probably lasts only for a time which is short
in comparison to the ejection variability period.
After the clump has completely merged with the jet head, the material
heated in the interaction will cool radiatively, first emitting a
high excitation spectrum, later emitting a lower excitation
spectrum, and finally fading away.
Interestingly, the cooling timescale depends on the inverse of the
density, and is strongly dependent on the shock velocity. For the
cm-3 (number) density range and
km s-1 velocity range relevant for
HH jets, the cooling timescale ranges from about one month
up to
yr (see, e.g., Hartigan et al. 1987). Since, the
ejection variability periods that have been estimated for HH jets
lie in the
yr range (Raga et al. 2002), it is clear
that models with a wide range of
might be
relevant for different HH jets.
We have presented a simple model (based on considerations of mass and momentum conservation) for the motion of the head of a variable jet. The ejection variability leads to the formation of discrete "clumps'' along the body of the jet, and these clumps catch up with the jet head, supplying it with mass and momentum from the jet beam.
Interestingly, for the case of a perfectly collimated jet (i.e., with
zero opening angle) moving into a uniform environment this model leads
to a full analytic solution, which illustrates the properties of this
kind of flow. The analytic solution shows that in the early evolution
of the flow, the head of the jet first advances with the velocity v0of the clumps, and then slows down (as it incorporates environmental
material) monotonically until it is caught up by the second clump.
The increased momentum gives the head a larger velocity, which then
decreases again as the head travels away from the source (see Fig. 3).
After the head has been caught up by
clumps, it has enough
inertia that it coasts along at a more or less constant velocity,
which is a function of the time-averaged properties of the jet
and of the environmental density (see Fig. 3 and Eq. (15)).
If one has a jet with a low value of
(see Eq. (6)), the jet head travels at a low velocity
(see Eq. (15)), and therefore has a low excitation bow shock.
At the times at which the clumps catch up with the jet head, the
emitted spectrum has "flashes'' of emission which result from the
dissipation in the clump/jet head interaction. For low
,
the shock velocities associated with this interaction will have a shock
velocity
,
therefore having a high excitation
spectrum.
These "flashes'' will last for the sum of the (short) interaction
timescale and the cooling timescale of
the shocked material. As discussed in Sect. 3.3, for the parameters
of HH jets it is definitely possible to have cooling timescales
(where
is the ejection variability period). For
such parameters, the emission of the jet head will have periods
of "quiescent'', low excitation emission separated by short-lived,
bright "flashes'' of high excitation emission.
This regime for the motion of the head of a variable jet is clearly interesting from the point of view of modelling low excitation HH objects. In the future, this scenario should be tested by attempting to model individual low excitation HH objects with full gasdynamical numerical simulations.
Another interesting possible application of our model is the observation of non-thermal radio emission associated with outflows from young stars (see, e.g., Rodríguez et al. 1989). Henriksen et al. (1991) have shown that this non-thermal emission could be associated with particle acceleration in fast shocks in HH jets. The present model, in which fast shocks are present only for short time-periods could reconcile the existence of non-thermal emission in regions in which a high excitation emission line spectrum is currently not observed.
Acknowledgements
We would like to acknowledge support from the CONACyT grants 36572-E and 41320 and the DGAPA (UNAM) grant IN 112602.