First terrestrial soft X-ray auroral observation by the Chandra X-ray Observatory
ABSTRACT Northern auroral regions of Earth were imaged with energetic photons in the 0.1–10 keV range using the High-Resolution Camera (HRC-I) aboard the Chandra X-ray Observatory at 10 epochs (each duration) between mid-December 2003 and mid-April 2004. These observations aimed at searching for Earth's soft () X-ray aurora in a comparative study with Jupiter's X-ray aurora, where a pulsating X-ray “hot-spot” has been previously observed by Chandra. The first Chandra soft X-ray observations of Earth's aurora show that it is highly variable (intense arcs, multiple arcs, diffuse patches, at times absent). In at least one of the observations an isolated blob of emission is observed near the expected cusp location. A fortuitous overflight of DMSP satellite F13 provided SSJ/4 energetic particle measurements above a bright arc seen by Chandra on 24 January 2004, 20:01–20:22 UT. A model of the emissions expected strongly suggests that the observed soft X-ray signal is bremsstrahlung and characteristic K-shell line emissions of nitrogen and oxygen in the atmosphere produced by electrons.
- SourceAvailable from: Marina Galand[Show abstract] [Hide abstract]
ABSTRACT: We discuss here the energy deposition of solar FUV, EUV and X-ray photons, energetic auroral particles, and pickup ions. Photons and the photoelectrons that they produce may interact with thermospheric neutral species producing dissociation, ionization, excitation, and heating. The interaction of X-rays or keV electrons with atmospheric neutrals may produce core-ionized species, which may decay by the production of characteristic X-rays or Auger electrons. Energetic particles may precipitate into the atmosphere, and their collisions with atmospheric particles also produce ionization, excitation, and heating, and auroral emissions. Auroral energetic particles, like photoelectrons, interact with the atmospheric species through discrete collisions that produce ionization, excitation, and heating of the ambient electron population. Auroral particles are, however, not restricted to the sunlit regions. They originate outside the atmosphere and are more energetic than photoelectrons, especially at magnetized planets. The spectroscopic analysis of auroral emissions is discussed here, along with its relevance to precipitating particle diagnostics. Atmospheres can also be modified by the energy deposited by the incident pickup ions with energies of eV’s to MeV’s; these particles may be of solar wind origin, or from a magnetospheric plasma. When the modeling of the energy deposition of the plasma is calculated, the subsequent modeling of the atmospheric processes, such as chemistry, emission, and the fate of hot recoil particles produced is roughly independent of the exciting radiation. However, calculating the spatial distribution of the energy deposition versus depth into the atmosphere produced by an incident plasma is much more complex than is the calculation of the solar excitation profile. Here, the nature of the energy deposition processes by the incident plasma are described as is the fate of the hot recoil particles produced by exothermic chemistry and by knock-on collisions by the incident ions.Space Science Reviews 08/2008; 139(1):3-62. · 5.87 Impact Factor
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ABSTRACT: While X-ray astronomy began in 1962 and has made fast progress since then in expanding our knowledge about where in the Universe X-rays are generated by which processes, it took one generation before the importance of a fundamentally different process was recognized. This happened in our immediate neighborhood, when in 1996 comets were discovered as a new class of X-ray sources, directing our attention to charge exchange reactions. Charge exchange is fundamentally different from other processes which lead to the generation of X-rays, because the X-rays are not produced by hot electrons, but by ions picking up electrons from cold gas. Thus it opens up a new window, making it possible to detect cool gas in X-rays (like in comets), while all the other processes require extremely high temperatures or otherwise extreme conditions. After having been overlooked for a long time, the astrophysical importance of charge exchange for the generation of X-rays is now receiving increased general attention. In our solar system, charge exchange induced X-rays have now been established to originate in comets, in all the planets from Venus to Jupiter, and even in the heliosphere itself. In addition to that, evidence for this X-ray emission mechanism has been found at various locations across the Universe. Here we summarize the current knowledge about solar system X-rays resulting from charge exchange processes.Astronomische Nachrichten 04/2012; · 1.12 Impact Factor
Article: X-rays from solar system bodies
First Terrestrial Soft X-ray Auroral Observation by
The Chandra X-ray Observatory
Anil Bhardwaj1,*, G. Randall Gladstone2, Ronald F. Elsner3, Nikolai Østgaard4
J. Hunter Waite, Jr.5, Thomas E. Cravens6, Shen-Wu Chang7,
Tariq Majeed5,9, and Albert E. Metzger8
1 Space Physics Laboratory, Vikram Sarabhai Space Centre, Trivandrum 695022, India
2 Department of Space Science, Southwest Research Institute, San Antonio, TX 78228, USA
3 NASA Marshall Space Flight Center, Space Science Branch, NSSTC/XD12, Huntsville, AL
4 Department of Physics and Technology, University of Bergen, Bergen N-5007, Norway
5 Department of Atmospheric, Oceanic, & Space Sciences, University of Michigan, Ann Arbor,
MI 48109, USA
6 Department of Physics & Astronomy, University of Kansas, Lawrence, KS 66045, USA
7 University of Alabama in Huntsville, NSSTC, XD12, Huntsville, AL 35805, USA
8 Jet Propulsion Laboratory, Pasadena, CA 91109, USA
9 Now at Department of Physics, American University, Sharjah, United Arab Emirates
*Corresponding author: Tel +91-471-2562330; fax +91-471-2706535; email:
Journal of Atmospheric and Solar-Terrestrial Physics, in press (2006)
See also Press Release by NASA (News release: 05-192) and CXC (RELEASE: 05-10)
on this paper :
“Chandra Looks Back At The Earth” - December 28, 2005
Northern auroral regions of Earth were imaged with energetic photons in the 0.1-10 keV
range using the High-Resolution Camera (HRC-I) aboard the Chandra X-ray Observatory
at 10 epochs (each ~20 min duration) between mid-December 2003 and mid-April 2004.
These observations aimed at searching for Earth's soft (<2 keV) X-ray aurora in a
comparative study with Jupiter’s X-ray aurora, where a pulsating X-ray “hot-spot” has
been previously observed by Chandra. The first Chandra soft X-ray observations of
Earth’s aurora show that it is highly variable (intense arcs, multiple arcs, diffuse patches,
at times absent). In at least one of the observations an isolated blob of emission is
observed near the expected cusp location. A fortuitous overflight of DMSP satellite F13
provided SSJ/4 energetic particle measurements above a bright arc seen by Chandra on
24 January 2004, 20:01–20:22 UT. A model of the emissions expected strongly suggests
that the observed soft X-ray signal is bremsstrahlung and characteristic K-shell line
emissions of nitrogen and oxygen in the atmosphere produced by electrons.
Key Words: Auroral emissions, X-rays, Chandra X-ray Observatory, electron
bremsstrahlung, Earth’s upper atmosphere, Jupiter.
Both Earth and Jupiter are magnetic planets having dense atmospheres and well-
developed ionospheres and magnetospheres (e.g., Schunk and Nagy, 2004; Bagenal et al.,
2004). Thus, several atmospheric, ionospheric and magnetospheric phenomena are found
to exist on these planets that are similar in nature, including auroral processes and
emissions (e.g., see reviews by Bhardwaj and Gladstone, 2000; Waite and Lummerzheim,
2002; Galand and Chakrabarti, 2002; Clarke et al., 2004). Both planets also exhibit X-ray
emission associated with their auroras and their non-auroral disks (Stadsnes et al., 1997;
Petrinec et al., 2000; Bhardwaj et al., 2002, 2006b; Waite and Lummerzheim, 2002;
Bhardwaj, 2006). It is well known that the X-ray aurora on Earth is generated by
energetic electron bremsstrahlung (e.g., Berger and Seltzer, 1972; Stadnes et al., 1997;
Petrinec et al., 2000; Bhardwaj et al., 2006b), and the X-ray spectrum of the aurora has
been very useful in studying the characteristics of energetic electron precipitation
(Stadnes et al., 1997; Østgaard et al., 1999, 2001). On the other hand, auroral X-rays from
Jupiter are mainly produced by charge-exchange of highly-ionized energetic heavy ions
precipitating from the outer magnetosphere and/or solar wind (Gladstone et al., 2002;
Cravens et al., 1995, 2003; Branduardi-Raymont et al., 2004, 2005, 2006b; Elsner et al.,
2005; Bhardwaj et al., 2006b; see review by Bhardwaj and Gladstone, 2000 for earlier
studies). Disk X-ray emission from both planets is largely due to scattering and
fluorescence of solar X-rays (McKenzie et al., 1982; Petrinec et al., 2000; Maurellis et
al., 2000; Bhardwaj et al., 2005, 2006a, 2006b).
Recent X-ray observations of Jupiter by Chandra X-ray Observatory (CXO) have
demonstrated that most of Jupiter’s northern auroral X-rays come from a ‘hot spot’
located poleward of the main ultraviolet auroral oval, thus pointing to a particle source
population in the outer magnetosphere (Gladstone et al., 2002; Elsner et al., 2005).
Interestingly, the hot spot X-rays pulsate with an approximately 45 (±20) minute period,
a period similar to that reported for high-latitude radio and energetic electron bursts
observed by near-Jupiter spacecraft (cf. MacDowall et al, 1993; McKibben et al., 1993;
Elsner et al., 2005). One possible explanation for the X-ray hot spot is high-latitude
reconnection of interplanetary magnetic field (IMF) lines, allowing the precipitation of
heavy solar wind ions into Jupiter's cusp region. Since the solar wind heavy ions are
highly ionized they can produce soft X-rays by charge exchange and excitation (i.e., the
same mechanism responsible for cometary X-rays, cf., Cravens, 2002) as they encounter
Jupiter's upper atmosphere.
The identical process should operate at Earth as well. However, while hard X-ray
emissions from electron bremsstrahlung are well known in the terrestrial aurora (i.e.,
Stadsnes et al., 1997; Østgaard et al., 2001), surprisingly, there have been no dedicated
searches for auroral X-ray emissions at energies <2 keV. A few limb scans of the
nighttime Earth at low latitude by the X-ray astronomy satellite, HEAO-1, in the energy
range 0.15 keV to 3 keV, showed clear evidence of the K-α lines of Nitrogen and Oxygen
sitting on top of the bremsstrahlung spectrum (Luhmann et al., 1979). Dedicated auroral
X-ray experiments have not measured X-rays below 2-3 keV, e.g., the PIXIE X-ray
imager on the Polar spacecraft measured X-rays in the range 3-60 keV (Imhof et al.,
1995). The high apogee of the Polar satellite (~9 RE) enabled PIXIE to image the entire
auroral oval with a spatial resolution of ~700 km. PIXIE data showed that the substorm
X-rays brighten up in the midnight sector and have a prolonged and delayed maximum in
the morning sector due to the scattering of eastward-drifting electrons (Østgaard et al.,
1999). Statistically, the X-ray bremsstrahlung intensity is largest in the midnight
substorm onset, is significant in the morning sector, and has a minimum in the early dusk
sector (Petrinec et al., 2000). During the onset/expansion phase of a typical substorm the
electron energy deposition power is about 60-90 GW, which produces around 10-30 MW
of bremsstrahlung X-rays (Østgaard et al., 2002).
We have conducted a series of short duration CXO observation of Earth aimed at
searching for soft (<2.0 keV) X-ray auroral emissions for a comparative study with
Jupiter’s X-ray aurora. In this paper we report the first observation of soft (0.1-10 keV)
X-ray emission from terrestrial aurora and present some of the preliminary results.
2. Chandra X-ray Observation of Aurora
Ten HRC-I (High Resolution Camera in imaging mode) observations were performed
when CXO was near apogee (~20 RE; Chandra moves in a highly elliptical 63.5 hr orbit)
and timed during northern winter of 2003-2004, so that the northern polar region was
mostly dark and solar fluoresced X-ray contamination could be avoided (cf. Table 1).
HRC-I is sensitive to X-rays in the 0.1-10 keV band (with a peak efficiency near ~0.6-2.0
keV) and has spatial resolution of 0.5″ (~0.3 km at Earth from Chandra apogee). Each
observation was ~20 min in duration (cf. Table 1), with fixed pointing in right ascension
and declination, arranged so that the parallax motion of the Earth allowed the north polar
cusp to drift through the HRC-I field-of-view (30′ × 30′, or about 1150 km × 1150 km at
the Earth as seen from Chandra apogee) at a variety of local times.
The time-tagged photon list data were analyzed with the CIAO software (v3.1) available
from CXO (http://cxc.harvard.edu/ciao/). Each observation was corrected for the Earth’s
motion and converted into brightnesses images using appropriate exposure maps. As the
mean photon energy is not known, a typical HRC-I effective area of 40 cm2 was assumed
in converting counts to Rayleighs.
These CXO-HRC-I observations (combined with a test observation taken on February 7,
2003, cf., Table 1) reveal a range of morphologies of X-ray auroras in the northern polar
region of the Earth. These first Chandra soft (0.1-2 keV) X-ray observations of Earth’s
aurora show that it is highly variable; they appear sometime as intense single arcs, other
times as multiple arcs, or as diffuse patches, and at times almost absent. Figure 1 shows
six examples of these different manifestations of the soft X-ray aurora. Generally, auroral
X-rays are brighter when Bz is negative for few hours prior to the Chandra observation.
In one of the observations an isolated blob of emission is observed (cf. Figure 1e) near
the location where we expect the cusp to be, perhaps giving an indication of solar wind
charge-exchange signature in X-rays. However, this identification is still tentative.
Figure 2 shows the CXO observation on 24 January 2004, 20:01–20:22 UT, when a
bright arc is seen. Unfortunately no good view of the aurora from IMAGE/FUV is
available at this time. TIMED/GUVI provided only a marginal view of this area about 20
min prior to the Chandra observation. However, the DMSP F13 flew over this region at
the same time that the HRC-I observed the bright arc. Taking advantage of this situation,
in the following, we calculate the X-ray emissions expected from bremsstrahlung and
characteristic K-shell line emissions of nitrogen and oxygen in the atmosphere produced
by the electrons measured by the DMSP F13 SSJ/4 electrostatic analyzers and compare it
with our HRC-I observation.
3. DMSP Observation and Electron Bremsstrahlung Model
The DMSP satellites are sun-synchronous polar orbiting satellites with orbital period of
101 min and a nominal altitude of 830 km. The satellites are three-axis stabilized, and the
detector always points toward local zenith. The SSJ/4 electrostatic analyzers on board the
DMSP satellites measure electrons and ions from 32 eV to 30 keV in 19 logarithmically
spaced steps (Hardy et al., 1984). One complete electron and ion spectrum is obtained
every second. At the latitudes of interest in this paper, this means that only particles at
pitch angles <15°, well within the atmospheric loss cone, are observed. To estimate the
X-ray production we have used 10 s averaged spectra from the SSJ/4.
In the energy range 0.1–2.0 keV there are two components to the X-ray spectrum
produced by electrons; the continuous bremsstrahlung spectrum and the strong K-α
emission lines from nitrogen (at 0.393 keV) and oxygen (at 0.524 keV).
To compute the X-ray bremsstrahlung production from electron precipitation, we use a
look-up table of the angular dependent X-ray spectra produced by single exponential
electron spectra. The look-up table is generated on the basis of the ‘general electron-
photon transport code’ of Lorence (1992). This code takes into account the scattering of
electrons, production of secondary electrons, angular dependent X-ray production,
photoelectric absorption of X-rays and Compton scattering of X-rays.
From previous studies of X-ray measurements it has been found that a sum of two
exponentials can often be used to represent the X-ray spectra very well [e.g., Goldberg et
al., 1982]. From a rocket experiment in the post midnight sector during the recovery
phase of a substorm (Østgaard et al., 1998), when both X-ray measurements and electron
measurements were available, it was found that both the electron spectrum and the X-ray
spectrum could be represented by a sum of two exponentials, giving very good
correlation when comparing measured and calculated electron spectra and measured and
calculated X-ray spectra. Figure 3 shows two-exponential fits to eight 10-s averaged
spectra measured by DMSP F13 (1959:55–2001:04 UT) as the satellite passed through
the arc observed by the Chandra. Using 15 of the 19 channels of the SSJ/4 detector we
obtain electron spectra from 0.1 to 30 keV. The double exponentials represent the
measurements fairly well, but the fit may be worse for energies above 30 keV. The
existence of a hard tail in the electron spectrum above 30 keV would lead to an
underestimate of the X-ray production. In some of the spectra such a hard tail can be
seen, but as the flux level falls off rapidly at the high energies, we do not expect the
contribution to the X-ray production to be very large. Keeping in mind that our approach
may lead to a slight underestimate of the predicted X-ray bremsstrahlung, we conclude
that the double exponential fit can be used to represent the electron measurements from
the DMSP satellite in the present study. A similar approach and conclusion was obtained
by Østgaard et al. (2000) when comparing estimated and observed X-rays from DMSP
and PIXIE, respectively, and we refer to that paper for further documentation on the
methodology used in the present study.
To estimate the production of the K-α emission lines we have used the results from
Luhmann and Blake (1977), where they have given the relative production of line
emissions and bremsstrahlung in a 100-eV band around these lines (cf. Figure 4 of
Luhmann and Blake, 1977). Folding these results with the DMSP spectra (Fig. 3)
measured over the X-ray arc, we find that the bremsstrahlung X-rays must be multiplied
by a factor of 4 to 6, depending on the shape of the electron spectrum.
4. Discussion and Summary
Figure 4 shows the time series of the calculated X-ray fluxes in the two energy ranges of
0.1–2.0 keV (middle panel) and 2.0–10 keV (bottom panel) calculated using the DMSP
F13 measured electron fluxes (shown in the top panel) on January 24, 2004. Most of the
X-rays (>~70%) are produced in the softer 0.1–2.0 keV X-ray band. The X-rays in the
0.1-2.0 keV band include both bremsstrahlung and characteristic line emissions of the
atmosphere. In a narrow energy band of ~100-eV around 0.4-0.5 keV, the K-α oxygen
and nitrogen line emissions are 30-50 times stronger than the bremsstrahlung. The X-ray
brightness from the brighter part of the arc seen in the HRC-I image (cf. Figure 2) is
estimated to be ~1 × 105 photons cm-2 sr-1 s-1. From Figure 4 we find that the energy-
integrated bremsstrahlung X-ray flux over the 0.1–10 keV range is likewise about 1 × 105
photons cm-2 sr-1 s-1 at the peak. This strongly suggests that the Chandra HRC-I observed
X-ray emissions on January 24, 2004 are X-rays (bremsstrahlung and line emissions)
from electron precipitation. Since the DMSP F13 satellite is not going through the cusp
region and the X-ray arc is basically in the post-noon/dusk sector (and not in the cusp) –
this is a very reasonable result.
It is interesting to note that most of the auroral X-rays at Jupiter are produced due to
charge exchange collision between precipitating highly-ionized heavy (O, S and/or C)
energetic (>1 MeV) ions and ambient neutrals in the polar upper atmosphere. These X-
rays are line emissions and arise as the heavy ions are nearly stripped of electrons while
precipitating, and then (through further collisions) are either directly excited or charge
exchanged into an excited state, which emits an X-ray photon upon decay back to the
ground state (cf. Cravens et al., 2003; Elsner et al., 2005; Bhardwaj et al., 2006b). Earth
auroral X-rays are known to be produced due to bremsstrahlung (and line emissions
(around 0.4-0.5 keV) at lower energies) by precipitating electrons, and the present study
suggests that even at softer (<2.0 keV) X-ray energies the source appears to be the same.
The spectrum of X-rays at these soft energies would help to further strengthen this
statement. The other possible source of Earth auroral X-rays could be the precipitation of
solar wind ions in the cusp region and production of X-rays in charge exchange collision
of highly-ionized heavy (C, N, O) solar wind ions with ambient atmospheric species. The
polar cusps are extremely dynamic regions that play a key role in the transfer of mass,
momentum, and energy from the solar wind into the magnetosphere and upper
atmosphere systems. It has been argued that cusp is an important source region of
energetic particles (Fritz, 2001; Chen and Fritz, 2005). Recently, it has also been
suggested that the solar wind ions can be energized at the Earth's bow shock before
entering the cusp (Chang et al., 1998, 2000). For high charge state ions (O+6), the energy
can be as high as 1 MeV (Chang et al., 1998, 2000). This is important, as observations at
Jupiter suggest that even solar wind ions need to be accelerated if they are to provide the
observed power of the auroral X-rays (Cravens et al., 2003; Elsner et al., 2005). In 10
April 2004 Chandra Earth observation we do see a spot of X-ray emission near (though
not very close) the calculated location of cusp (cf. Figure 1e). However, in the absence of
an X-ray spectrum of this emission-blob, and the lack of proper ion flux measurements, it
is difficult to decipher the possible source mechanism. We will propose to conduct
observations in the future using Advanced CCD Imaging Spectrometer instrument on
Chandra or with XMM-Newton that both have spectral resolution to distinguish between
line emissions from highly-charged ions and continuum (cf. Elsner et al., 2005;
Branduardi-Raymont et al., 2005, 2006).
This work is based on observations obtained with Chandra X-ray Observatory and was
supported by grant from the Chandra X-ray Center. A part of this research was performed
while A. Bhardwaj held a National Research Council Senior Resident Research
Associateship at NASA Marshall Space Flight Center. We acknowledge the excellent
help we received from Michael Juda of CfA in performing these Earth X-ray
observations with Chandra. We also acknowledge help from Johan Stadsnes in locating
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Table 1. Log of Observation by the Chandra X-ray Observatory
07 February 2003 4410
IMF By, Bz2
16 December 2003 4456 04:14 04:35 1.3, 1.6 -33.7
06 January 2004 4457 07:57 08:18 0.6, -1.8 -29.4
24 January 2004 4459 20:01 20:22 -4.9, -3.8 -12.2
30 January 2004 4460 03:06 03:26 7.2, 2.4 -27.1
14-15 February 2004 4461 23:58 00:18 -2.5, -1.4 -15.8
28 February 2004 4458 05:01 05:22 8.6, -2.4 -18.6
04 March 2004 4462 12:04 12:32 2.3, 0.4 -2.7
07 March 2004 4463 03:32 03:53 2.7, 0.7 -14.9
10 April 2004 4464 12:28 12:48 1.3, 2.0 +12.9
13 April 2004 4465 03:46 04:07 -2.7, -1.2 -0.9
1hh:mm in UT.
2The IMF (interplanetary magnetic field) By and Bz are in GSM (Geocentric Solar
Magnetospheric System) coordinates
observation times from the hourly averaged-values.
3Dipole tilt is defined as the angle between the Earth’s north dipole axis and the GSM z-
axis (cf. Zhou et al., 1999). This angle is positive when the dipole tilts towards the Sun,
and negative when the dipole tilts away from the Sun.
to Chandra and
Figure 1. Six example X-rays images (shown on the same brightness scale) of the north
polar region obtained by Chandra HRC-I on different days (marked on top of mages),
showing large variability in soft (0.1-10.0 keV) X-ray emissions from Earth’s aurora.
Note that the images are not snap shots, but are ~20-min scans of the northern auroral
region in the HRC-I field-of-view. The brightness scale in Rayleighs (R) assumes an
average effective area of 40 cm2. 1 R = 106 photons cm-2 s-1 (4πsr)-1. Black crosses and
asterisks mark the day-night terminator (shadow boundary) at an altitude of 0 and 100
km, respectively. Green diamonds indicate the noon/midnight MLT meridian at an
altitude of 100 km. A green triangle marks the magnetic pole and a green asterisk marks
the expected cusp location. The location of cusp is calculated using relations given in
Newell et al. (1989).
Figure 2. Chandra HRC-I X-ray image of auroral region on January 24, 2004 showing a
bright arc. The orbital location of satellite DMSP F13 is shown by red diamonds, with 2-
minute time ticks and vertical lines extending down to an altitude of 100 km. Other
symbols and descriptions are as in Figure 1.