The Earth’s atmospherejorge/aga5802_2017/2017_06_atmosfera_terr… · Structure of Earth’s...
Transcript of The Earth’s atmospherejorge/aga5802_2017/2017_06_atmosfera_terr… · Structure of Earth’s...
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The Earth’s atmosphere
www.pbase.com/psinclai/la_silla Prof. Jorge Meléndez
Bibliography: Lena’s book (chapter 2) and other sources, p. ex., livro Meteorology Today (Ahrens)
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Most observations are performed on the ground
www.nasa.gov
We must know the
Earth atmosphere to
understand the limitations
for ground observations
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Earth’s
is a fine layer of gas that surrounds Earth and that is kept by gravity
atmosphere
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© Meteorology Today (Ahrens)
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Structure of Earth’s atmosphere b
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Temperature profile
TROPOSFERA
MESOSFERA
ESTRATOSFERA
TERMOSFERA
Warm by the ground and convection
Warm by ozone UV absorption
Solar UV light and X-rays heat and ionize gas
Ozone decreases
TEMPERATURE(0C)
Alt
itu
de (
Km
)
X-ray UV visible
570 HST
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Pressure: decrease exp. with height z
H: height scale (=RTm/M0g)
Chemical composition aprox. constant until 90 km
P(z) =
P0exp(-z/H)
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H=RTm/M0g
(scale height)
R: gas constant (8.23 J K-1 mol-1)
Tm: mean temp. (00 C)
M0: mean mol. mass (0.029kg)
g: gravity
H = 8km
P(z) = P0exp(-z/H)
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Which are the main constituents of the atmosphere?
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Constituents of the atmosphere
N & O are the main constituents and its proportion is relatively constant between 0-90 km
Nitrogen (N2 : 78 %)
Oxygen (O2 : 21 %)
Argônio (0.9 %) (H2O, O3, …) Vapor de agua é varíavel, ~1%
(CO2: 0.04 %)
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Constituents of the atmosfera The minor (and variable) constituents are important sources of opacity in the atmosphere
(CO2 , H2O, O3,…) w
ww
.co
smic
dia
ry.o
rg
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Water vapor: one of the most important sources of opacity
© Meteorology Today (Ahrens)
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Measurement of the water vapor content The fractional content, mixing ratio, or specific humidity is:
•0 < r ≤ rs(T) (saturation)
Very sensitive to: • Temperature • z (altitude) • Latitude • time
[r] = g/Kg
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Mass concentration of water vapor per volume of saturated air at normal pressure as a function of
temperature Tem
pera
ture
(OC
)
g(H20) per m3 of air
© Lena
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latitude
Mixing ratio as a function of latitude
© Meteorology Today (Ahrens)
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Concentration of water vapor as a funtion of altitude
© Lena
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Precipitable water
Precipitable water above
altitude z0 :
where is the number of molecules/volume
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Column of precipitable wapor vapor
where ρ0 is air density at z0
r(z) changes rapidly: scale height of water vapor is
(3km) << dry air (8 km)
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Comparison of water vapor at 2 diferent observatories
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Keck (4.2km) spectrum of HD140283
Stellar NaD
Interstellar NaD
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Keck (4.2km) vs. VLT (2.7km)
ISM NaD
Stellar NaD
Water
vapor
clearly
present
on
Paranal
(VLT)
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Keck (4.2km) spectrum of HD140283
Stellar NaD
Interstellar NaD
much
less H2O
on Mauna
Kea
(Hawaii)
than on
Paranal
(Chile)
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Umidade relativa (Relative humidity: RH)
RH = water vapor content
Maximum water vapor content for saturation at a given T
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RH = Water vapor content
Maximum water vapor content for saturation
© Meteorology Today (Ahrens)
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Variation of relative humidity during the day ©
Me
teo
rolo
gy T
od
ay (
Ah
ren
s)
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Change in RH on 5/mar/2014 OPD observatory
18h: 70% 20h: 80% 22h: 90% 0h: 100%
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Change in temperature and RH on 9/3/2014 te
mp
era
ture
R
ela
tive
hu
mid
ity
time
time
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Change in temperature and RH on 9/3/2014 te
mp
era
tura
R
H
time
time
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Cloud coverage 9-10/3/2014
time
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Ozone (O3) Vertical structure of O3 changes a lot (latitude,
season of the year), but maximum ~20km
Stratospheric
Ozone
Tropospheric ozone
Andrew Ryzhkov
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Ozone (O3) Northern hemisphere has larger concentration
of ozone
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Ozone (O3) Zone O3 has an annual cycle
Mar Apr Oct Nov
Tipically 0.24-0.34 cm
in STP
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Ozone: principal protection for UV solar radiation
100%
90%
10%
100-280nm
280-320nm
320-400nm UV-C
UV-B
UV-A
0.2 .3 .4 μm
C B
A
Altura
(km
)
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Ozone destruction
• Minor constituents (Cl, NO) destroy O3
• Cloroflour-carbonates, CFCs, can reach the stratosphere and destroy ozone
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Carbo dioxide
• Similar distribution to O2 e N2
• Mixing ratio does not depend on altitude
• Important source of absorption in the infrared
CO2
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CO2 and global warming
CO2 is the second source of global warming (after H2O)
Visible light pass through atmosphere and heats the surface. Gases (CO2, H2O & CH4) in atmosphere absorb the reflected IR light, re-emitting in random directions
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CO2 and global warming
CO2 in the last 1000 years
© Meteorology Today (Ahrens)
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CO2 and global warming
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CO2 and global warming
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Impact on Astronomy Rise of CO2:
deeper
absorption
bands in the
atmosphere
Atmospheric absorption bands
(telluric bands)
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Impact on Astronomy?
Dec-Feb Jun-Aug
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Ions •Above 60km, solar UV radiation ionizes the atmosphere
•Ionization changes with altitude, solar illumination, solar activity
•At high latitudes, electron cascades enter magnetic poles,
causing auroras
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Ions : Auroras •Acima de 60km, radiação solar UV ioniza a atmosfera
•A Ionização varia com altitude, iluminação solar, ativ. solar
•A altas latitudes, “cascatas” de elétrons entram nos polos
magneticos, causam as auroras
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Ions •Typical reactions:
• Variation of eletronic densities:
Layer z(km) Ne[cm-3]
D 60 103
E 100 105
F 150-300 2x106
> 2000 104
•D almost dissapears at night
•Interference in radio waves
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Ionospheric plasma Ionized layers have an index of refraction n related to the electron density Ne
•n2 = 1-ωp2/ω
= 1-(λ/λp)2
•νp[Hz] = ωp/2π
=9 x103Ne1/2
For F layer (Ne = 2x106 cm-3), λp=23.5m (νp=12 MHz)
Total internal reflection
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Absorption of Radiation The absorption by the atmosphere could be total or
partial
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Atomic and Molecular absorption
Atomic: O, N
Molecular:
• Electronic
CH4, CO, H2O, O2, O3, …
• Rotacional:
H2O, CO2, O3, …
• Vibrational-Rotational:
CO2, NO, CO … Eel,v”,J” = [Te + Gv + Fv(J)] hc
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Atomic & molecular physics gives κ or σ for each species
Atmospheric absorption bands Telluric bands
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In the optical and near infrared, O3, H2O & CO2 cause strong absorption bands in Earth’s atmosphere
Solar spectrum & telluric bands
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At the near infrared, H2O cause strong absorption bands in Earth’s atmosphere
γ Cas and telluric bands
J H K
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Atmospheric transmission
0.9 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 2.0 2.1 2.2 2.2 2.4 2.5 2.6 2.7
2.8 3.0 3.2 3.4 3.7 4.0 4.2 4.4 4.6 4.8 5.0 5.2 5.4 5.6
6 8 10 12 14 16 18 20 22 24 26 28 μm
Mauna Kea com H2O = 1mm(1mm) & 3mm
www.gemini.edu
J H K
L M
N P
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Water Vapor: Mauna Kea vs OPD
Mauna Kea
h(1mm ,3mm)
OPD/LNA
h(10mm) Barbosa(2000)
OPD/LNA
h(20mm) Barbosa(2000)
1.0 1.5 2.0 2.5 λ
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Optical depth The optical depth along a vertical line, of a constituent
i with mixing ratio ri(z) is:
The attenuation of an incident ray of intensity I0 (top of the
atmosphere) received at altitude z0 and at an angle θ from the
zenith, is:
The sum is over all species that absorb
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Atenuation of radiation with altitude
Atmosphere
totally
opaque for
τ = 10
Ideally
observatories
are feasible
for τ < 0.5
(transmission
> 61%)
τ = 0.7
2.3
4.6
I/Io
= 1/2
1/10
1/100
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Ground-based observatories
Far UV (<20nm)
Near UV
Continuum N2
Elect bands O2 , O3, cont O2
IR & sub-mm
Bands (rot. & v-r)
H2O e CO2
mm
Rot. bands H2O & O2
10-20m
cutoff
Ionospheric plasma
Optical –
IR window
Radio
window
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ALMA: 66 antennas working together at mm and submm
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Atmospheric emission
• The atmosphere emits by
florescence (airglow) & termically
FLUORESCENCE: recombination of e- & ions from diurnal dissociation; ex.:
• Continuum: 1-3 Rayleigh Å-1
• Lines: 500 R 1 Rayleigh (R) = 106 photons cm-2 s-1 str-1
= 6.8x10-17 Wm-2um-1arcsec-2(em =550nm) = 22 mag arcsec-2
• Main emitters: OI, NaI, O2, OH, H
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Spectrum of the night sky (optical) Mauna Kea (Hawaii)
www.cfht.hawaii.edu
O2
Hg
[NI]
5199
[OI] 5577
[OI]6300,6363
OH
OH
OH OH
HI
NaI 5890;6
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Spectrum of the sky at night (optical & infrared)
Observatory La Palma (Canary Islands)
OH is very strong
in the red and
infrared
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Sky background for observations on ground and space near Earth
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Co
nv
ec
tio
n
Thermal emission (infrared)
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Thermal emission • Atmosphere could be considered a gas in LTE until
40-60km
• For τ << 1 (shallow optical depth), the intensity of
radiation at altitude z and zenithal distance θ, is:
Bλ : Planck function at mean temperature T of the
atmosphere
τ << 1 and Bλ non-negligible, satisfied for:
- Infrared window: 1 - 20 μm
- Milimeter window: 0.5 – 2 mm
¯
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Thermal emission Using a mean temperature 250K:
Astronomical
sources could be
several orders of
magnitude weaker
than sky thermal
emission (also
could be
problematic for
sky fluorescent
emission).
Léna, Lebrun & Mignard 1998
Observational astrophysics, 2nd Ed
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Sky background in the infrared: thermal emission vs. OH
Sky background emission in the infrared, at the altitude of
Mauna Kea (4200m).
Fluorescent
emission (OH)
Thermal
emission
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Scattering of radiation: Rayleigh & Mie
• Caused by molecules and aerosols in suspension
• Influence of ar molecules depends on altitude, but aerosols depend on winds, weather, season, volcanic activity, industrial pollution
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• For particles smaller than the light wavelength λ:
• n: refraction index;
• N: density of molecules
Rayleigh scattering
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This is why the sky is blue
Rayleigh scattering also depends
on the incident angle θ: At z=2km: at 900 from the
Sun, λ=7000A, sky brightness
is 10-7 of the Sun’s disk
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Mie scattering • Scattering by particles larger than λ of light
• Does not depend much on wavelength
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Mie scattering
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Sky brightness during the day in the optical and
infrared Fig. 2.11 (Lena, Observational
Astrophysics). Molecular scattering is
given for the altitude z = 2000m, at 900
from the Sun. The wavelength
dependence is λ-4. Thermal emission
is also shown, assuming uniform
mean emissivity of 0.1.
The dashed line shows the possible
additional contribution due to aerosols,
varying as λ-1. For comparison, (•)
marks the sky brightness measured at
0.5 arcmin from the Sun’s limb at Kitt
Peak (Arizona)
Possible to
observe at
day or
night
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Other atmospheric factors: Atmospheric turbulence V
ince
nt
van
Go
gh
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Sources of turbulence by different obstacles
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Other atmospheric factors: inversion layer
• Important factor to choose an astronomical site
• Inversion layer ~ 2km, but
could occur at lower z
São Paulo, 6af, 23 maio 2008, 08h30m www.estadao.com.br
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Inversion layer Inversion layer above the pacific ocean around the Big Island of Hawaii
www.gemini.edu
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High altitude less clouds
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Brazilian students @ La Silla, 20/9/2013
Meteorological conditions at La Silla (Chile)
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1/10/2013
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Pointing with limitations
Close
Direction
of the
wind
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La Silla, 22/9/2013
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Dome-Closing Conditions at ESO LaSilla
Humidity. General humidity sensors are installed on the weather tower; their
readings are relayed on the MeteoMonitor . Domes have to be closed
when the relative humidity exceeds 80% (was 90%),
and can be re-opened when it remains below 70% for
30min. Similarly, the domes must be closed when the temperature difference
between the coldest part of the telescope and the dew point drops below 2
degress. https://www.eso.org/sci/facilities/lasilla/sciops/At_Telescope.html
< 14 m/s
< 14-20 m/s
> 20 m/s (18 m/s for 3,6m)
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Hawaii
Hawaii, 18/8/2013
Mauna Kea mountain
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Mauna Kea Weather conditions
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Choosing an astronomical site • No clouds (related to inversion layer)
• Photometric quality (atmospheric transparence)
• Transparence in the infrared & mm (atmospheric H2O)
• Image quality (related to variations in temperature and the air refraction index)
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Choosing an astronomical site
Altitude
precipitableH2O
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Choosing an astronomical site Cloud coverage
BEST SITES
High
summits
+ low
cloudiness +
low
precipitable
water vapor
Peru, Chile,
Bolivia,
Argentina
Sarazin 2006, IAU Symp 232
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In some cases we must go to space …