Heureux qui, comme Ulysse…

Heureux qui, comme Ulysse, a fait un beau voyage,
Ou comme cestuy-là qui conquit la toison,
Et puis est retourné, plein d’usage et raison,
Vivre entre ses parents le reste de son âge !

Quand reverrai-je, hélas, de mon petit village
Fumer la cheminée, et en quelle saison
Reverrai-je le clos de ma pauvre maison,
Qui m’est une province, et beaucoup davantage ?

Plus me plaît le séjour qu’ont bâti mes aïeux,
Que des palais Romains le front audacieux,
Plus que le marbre dur me plaît l’ardoise fine :

Plus mon Loir gaulois, que le Tibre latin,
Plus mon petit Liré, que le mont Palatin,
Et plus que l’air marin la douceur angevine.

Joachim Du Bellay- Les Regrets, sonnet XXXI, 1558

Why are drilling expeditions so important?

When you want to study rocks, one of the main complications is to access to them! Most of the time, they are hidden by soil and plants on land and of course, by the water in oceans!

To deal with that problem, geologists have developed indirect ways to image the underlying rocks by using sound waves (called seismic waves) which are generated mechanically. The data collected during these seismic surveys provides accurate information to “see” buried features.

Many seismic surveys have been conducted in the Ross Sea, so scientists already have some idea of the geological history of that region over the last millions of years. The image above is from a US seismic survey that took place in 1990 (Courtesy of Prof. John B. Anderson, Rice University).

What is a seismic survey?

The idea is to use waves which are able to go through the water and the sediments and rock below. A sound wave is created by an “air gun” that is towed from a ship, just below the surface of the water. The acoustic waves travel down through the water and some of them travel into the layers of sediments beneath the sea floor.

When the waves meet a hard surface (the sea bed or a different type of sediment for example), some waves are reflected (which means that they come back toward the sea surface) and only some continue to travel down into the sediments and into the rocks, until they became too weak and the initial seismic energy is dissipated. On the drawing below, only the rays of reflected waves are shown for simplicity.

The reflected waves are recorded by an array of geophones attached to a cable towed by the ship. These arrays are called “streamers” and consist of long net-like bands with hydrophones (sort of like underwater microphones) spaced evenly along the streamer.

Principle of a marine seismic survey (figure modified from L. De Santis U. Tinivella, OGS)

An animation is available here.

The information gathered by the geophones are then processed in order to obtain a seismic profile that can be analyzed by geologists.

Many seismic surveys have been conducted in the Ross Sea. This is an example of one of the seismic profiles obtained in 2005 under the Italian Antarctic Research Program (PNRA).

Example of a seismic profile collected in 2005 in the Ross Sea (Antarctica) with the R/V OGS Explora (Böhm et al., 2009)

A seismic profile provides a lot of information to scientists at a regional scale. For example, they can map faults and major lithologic units, interpret depositional environments and infer the lithofacies and the ages of different units.

In the example below, we can assume that the orange layer is a sedimentary wedge that has formed below and in front of an ice sheet (represented here in blue) that was grounding on the sea floor, stripping off sediments and entrain them into the basal ice and finally drop them at the ice front.

Partial interpretation of the previous seismic profile (Böhm G et al., 2009)

Why are drilling expeditions so important anyway?

Because even if a seismic profile provides crucial knowledge of large-scale geological structures, it is different from a real geological cross-section in many ways:

–  layers in a seismic section are imaging changes in surface reflectivity (eg density change) that are not always caused by a change of lithology, but they may be due to presence of fluid, gas, etc…

– more important, the vertical scale of the image is not the actual depth but it is time  (the time corresponding to duration of the travel of the sound waves from the ship to the sediment layers and backward to the geophones)

The results of interpretation of seismic profiles need to be verified with drilling data in order to enhance the accuracy of the interpretation. What make drilling expeditions crucial is that they can provide the missing information needed to have a complete story of the area (real depth, age, rock type [lithology], etc.). But drilling is expensive and time consuming, therefore it is crucial to plan the best site locations by conducting seismic surveys before drilling. Only after having carefully studied the geometry of the strata buried below the sea floor can we confidently drill down to the target. This is also the main technique employed by industry to look for oil and gas reservoirs in hidden “sediment traps”.

 

 

Expedition 374 and ice sheet modelling Conversation with Benjamin Keisling, scientist onboard the JOIDES Resolution during Expedition 374

Benjamin Keisling, scientist onboard the JOIDES Resolution during Expedition 374

Benjamin, can you please introduce you and explain your research topics?

My name is Benjamin Keisling and I am part of the Sedimentology team onboard Expedition 374. I am a PhD Candidate in Geosciences at the University of Massachusetts Amherst in the USA.

My PhD research centers on ice sheet modelling, and is particularly focused on how we can use proxy data to constrain uncertain processes and parameters in ice sheet models.

In other words, I use geological data to test how well ice sheet model simulations represent the past. The models that best represent the available geologic data can then be used with more confidence to make future predictions of sea level rise.

It is commonly accepted that big changes in the past sea levels are linked to variations of the volume of the Antarctic ice sheet. Is that true, and in that context, how important is it to have a better knowledge of these past variations?

Big changes in past sea levels certainly reflect variations in the volume of the Antarctic ice sheet, and accurate prediction of future sea levels relies on better knowledge of these past variations.

For example, we often use the most recent warm “interglacial” period in Earth’s history (the Eemian, 125 thousand years ago) as an analogue for the present because the amount of carbon dioxide in the atmosphere was similar to preindustrial levels (around 280 parts per million). However, sea level records indicate that during the Eemian sea levels were 6–9 meters higher than they are today, which means that part of Antarctica must have melted.

But it’s very difficult from a modelling perspective to make enough of the ice sheet melt to explain those sea levels, so it means that our models are missing something, and that affects our ability to confidently model how the ice sheet will respond to warming today (when carbon dioxide levels are greater than 400 parts per million!) and into the future.

Benjamin the modeler at work

On board, sedimentologists use the lithologies of the cores to estimate advances and retreats of the ice sheet during periods warmer than today, especially during Miocene and middle Pliocene. Can you explain how these data will be helpful in your work?

We know from many records that the size of the Antarctic ice sheet has fluctuated in the past, and models do a good job of recreating some of that variability. However, we are still lacking fundamental knowledge about what caused the ice sheet to retreat during past warm periods, and the sediments we are collecting can give us insight into that.

In Antarctica today, the ice mostly loses mass at its floating ice shelves (like the Ross Ice Shelf), where icebergs calve off and warm ocean waters melt the underside of the ice. Because Antarctica is so far south, it rarely melts from the surface – it stays below freezing even during the summertime. But there is a big debate now about whether the large variations in the size of the ice sheet are triggered by melting from the ocean or melting from the atmosphere.

Through studying the sediments we are collecting on Expedition 374, we will get a better idea of what the oceanic and atmospheric conditions were like before the ice sheet retreated, and this gives us information we can use to evaluate our models. In addition, it is notoriously difficult to constrain how certain parameters in our models have changed throughout geologic time, for example, the shape of the ice-sheet bed or how slippery it is. The sediments that we are describing can give us direct insight into these important parameters, so that our models have a better shot at getting the right answers for the right reasons.

We want to know how the sea levels will evolve in the future. And Expedition 374 is looking 25 My behind us! How can having a better knowledge or our past help us to predict the future when the atmospheric CO2 concentration will increase?

Geological data provide an invaluable source of information for models, because they give us targets to test models against. We don’t know exactly what will happen in the future, but geological data can tell us what happened in the past, and right now, the future is looking more and more like the Miocene and middle Pliocene. The amount of carbon dioxide in Earth’s atmosphere hasn’t been as high as it is today since at least the middle Pliocene, and during that time the ice sheet was probably smaller and very dynamic, causing oscillations in sea level on the order of 10 meters. We need to understand what drove these oscillations and how they affected the rest of the global climate system in order to predict when and how they will happen in the future.

If you want to learn more about what is a numerical modelling of ice sheet, you can visit this webpage:

http://www.antarcticglaciers.org/glaciers-and-climate/numerical-ice-sheet-models/

An example of ice-sheet numerical modeling is available here:

Le paléomagnétisme pour les Nuls- Partie 2

From last time, it seemed like studying Earth’s ancient magnetic field was not so complicated, right?

Oh, but maybe I omitted a few important details about how the paleomagnetists on board have to deal with some complications… Their ultimate target is to determine the age of the sediment. They do that by determining the polarity of Earth’s magnetic field: sometimes, it is normal (like today), sometimes it is reversed. The paleomagnetists measure the inclination (the dip of the magnetic field) specifically to determine the polarity of the field. They want to know whether the field goes into or comes out of Earth. In the southern hemisphere, the field comes out of Earth when the polarity is normal and the inclination is negative, and it goes into the Earth when the polarity of the field is reversed, during which the inclination is positive. Saiko and Tim are therefore always trying to figure out what the inclination of the sediment is.

However, this is not straightforward. When the cores arrive on deck and then into the hands of our paleomagnetists, there are more magnetic directions present in the core than just the one of the ancient magnetic field…

To make it simple, you can consider that there are 2 types of magnetic particles: the “good” ones and the “bad” ones. Yes, just like in a cowboy movie… The good ones are magnetically hard and are not disturbed by the small magnetic fields present during the drilling operations. The “bad” ones are magnetically soft. They align in the direction of every small magnetic field that is present during their trip from under the seafloor to the paleomagnetists’ lab.

Orientation of the magnetic particles in a sample after drilling. The field caused by drilling is usually pointing down. Hard particles do not align to that drilling field, but all soft particles changed orientation

All “soft particles” thus carry an paleomagnetic signal that is linked to the coring. This “overprint” is not useful when Tim and Saiko try to determine the direction of the ancient magnetic field. This overprint is sometimes so strong that it masks the original signal of the strong particles!

Our paleomagnetists have to remove that overprint to get to the real signal.

The problem is that most natural samples contain a combination of soft and hard magnetic particles… Our paleomagnetists want to get rid of the weak particles! How? They can’t dig out the bad particles, because then they would destroy the core and change the orientation of the good ones as well! They have work out a non-destructive method!

How does it work?

The big idea is to cancel out the overprint magnetization of the soft particles in order to only measure the magnetization of the hard ones. Remember that the soft ones are very susceptible to small magnetic fields. We can therefore change the orientation of the weak particles by applying a small magnetic field. This is similar to what happens in the drill string. Now we need to find a way to randomize the orientation of the soft particles so their combined effect is zero.

We do this by demagnetizing our samples, using an alternating magnetic field. This means that we generate a field that very quickly switches in direction whilst slowly dissipating to zero. This field is so small that it only affects the soft particles and not the hard ones. Depending on the properties of the soft particles, they align with the field at different times throughout the demagnetization.

The result is that all soft particles are now aligned in random directions so that their combined effect is zero. Fortunately, the magnetically hard particles don’t care about this small field and their magnetization does not change, which means these particles still have a record of Earth’s ancient magnetic field. So, the only signal we have left is the good one!

Orientation of the magnetic particles in a sample after demagnetization. All soft particles are now randomly oriented whilst the hard particles are still in their original orientation

It is now time to analyze some measurements made by our team during Expedition 374. Please read again our first post of “Paleomagnetism for Rookies” for all details about inclination and the polarity of Earth’s magnetic field.

This is an example of how a drilling overprint influences the real signal in sediments. The blue line is the inclination before demagnetization. You can see that all inclination values are positive. Remember that we are still drilling on the South Hemisphere close to Antarctica. Does that pattern mean that this sample was deposited during a period of reversed polarity?

No. Tim and Saiko demagnetized the sample and removed the drilling overprint. You can see that the inclination is now negative. This means that the sediments were deposited during a period of normal polarity!

Conclusion: Don’t judge a book by its cover; read its contents first. Similarly, don’t interpret the magnetic polarity without first removing overprints. Only then will the secrets of the past be revealed!

Saiko and Tim are happy with their magnetometer

Do you want to be part of the physical properties’ team on the JOIDES Resolution?

Have a look at this blog post!

Some physical properties of the cores and what they can tell us about sediments

Earth has experienced many cycles of climate change throughout its geologic history. Records of these past climates can be found in the sediments that we drill during Expedition 374. In order to learn more about past climatic conditions, we have to decipher the information recorded in the cores.

Scientists on board the JOIDES Resolution try to steal some of the secrets of the cores by measuring the physical properties of the sediments.

What are the physical properties measured on board the JOIDES Resolution? What kind of information can they provide?

  • “Magnetic susceptibility”

Magnetic susceptibility is the degree to which a material can be magnetized in a small external magnetic field (not exceeding 0.5 mT).

Magnetic susceptibility is an indicator for changes in the composition of the sediments. Sediments can come from the erosion of rocks on the continent (terrigenous sediment such as sand and clay) and/or they can have a biogenic origin (which means that they form from the remains of once living organisms that die and fall to the seafloor, the test (shells) of plankton for example).

The range of magnetic susceptibility values gives us an idea of the proportion of terrigenous versus biogenic particles, which is a clue for their source. If the sediment is mainly composed of terrigenous particles, the magnetic susceptibility will be higher than if the sediment is mainly biogenic, when magnetic susceptibility will be close to zero.

  • “Gamma ray attenuation bulk density”

Bulk density is a measure of mass per unit volume (g/cm3).

This measurement uses a gamma ray radiation, which interacts with the sediment or the rock. The attenuation of gamma radiation is linked to the density of the material: the stronger the attenuation, the denser the sediment.

Changes in density are also linked to the porosity of the sediments which represents the volume of the open spaces between sediment/rock grains compared to the total volume of the rock.

A change in the bulk density is often an indicator of changes in the type of sediments (mineral composition, grain size, etc.…).

  • “Natural gamma radiation”

Some radioactive isotopes (uranium, thorium, and potassium) are present naturally in some sediments. Thorium and potassium are usually found in clays, whereas uranium is present in clays and organic-rich materials. Gamma rays are emitted spontaneously from atomic nuclei during radioactive decay and this natural radioactivity is recorded by the “Natural Gamma Radiation Logger” on the JOIDES Resolution.

In general, the natural radioactivity is a useful tool to measure the amount of clays in the sediments.

You are now ready to be part of the physical properties’ group on the JOIDES Resolution! These are some results that we record during Expedition 374. It is your turn to play!

Question A: Using the magnetic susceptibility, which sediments have a higher content of terrigenous particles:

  1.  sediments from period 1
  2. sediments from period 2
  3. both have the same content in clays

Question B: Using the record of gamma ray attenuation bulk density, we can say that the sediments from period 1 have:

  1. higher porosity than those of period 2
  2. the same porosity as those of period 2
  3. lower porosity than those of period 2

Question 3: Using the natural gamma radiation, we can say

  1. sediments of period 1 have higher clay content than those of period 2
  2. sediments of period 2 have higher clay content than those of period 1.
  3. sediments of period 1 have the same clay content as sediments of period 2

Answers: A.2 ; B.3 ; C.2

All your answers were correct? Well done!

The sediments of period 1 are diatom-rich mud formed mainly by accumulation of diatoms and with high porosity. They are deposited in open-water conditions which are good for the proliferation of diatoms.

The sediments of period 2 are diamictite. They form by accumulation of terrigenous sediments brought by the ice sheets and have a high content in clay, sand, and gravel. The climate was much colder than during period 1 as the same location was covered by an ice shelf.

We can conclude that the passage from sediments of period 2 (older) to sediments of period 1 (younger) is linked to warming temperatures.

Now you are ready to apply for an expedition on the JOIDES Resolution !

 

 

 

A hole in the ship?

During Expedition 374, the moonpool was fully opened to lower the subsea camera system to the sea floor.

I have always heard about Archimedes’ principle and I know that it explains why heavy ships like the JOIDES Resolution (145 m long and 21 m wide) can float on the water without sinking. But, I didn’t think that it could be compatible with the presence of a hole like the moonpool in the bottom of the ship!

When I saw that opening the moonpool in the ship didn’t change anything, I was very confused.

What? There is a hole in the ship and she doesn’t sink? How is it possible?”

Video music by Mark Teckenbrock. Video by Kim Kenny. 

 

And again, I had to ask for some help from a physicist.

First of all, we must understand Archimedes’ principle. The reason why ships don’t sink is known as Archimedean buoyant force.

Archimedes’ principle states that the upward buoyant force that is applied on a body immersed in the water is equal to the weight of the body. The ship, because of her weight, tends to sink by gravity. A consequence of Archimedes’ principle is that the water under the ship applies a counter pressure on it. This counter pressure is the same amount as the pressure from the weight of the ship but it is in the opposite direction and prevents the ship from sinking!

Physicists say that the ship is in a hydrostatic balance state (it means that she floats….)

But why doesn’t the opening of the moonpool fill the ship with water?

The moonpool is an opening that is 6.7 m in diameter in the center of the ship that gives access to the water below. We opened it during Expedition 374 because we wanted to lower the camera system.

And…it surprised me (it wasn’t the first time I saw the opening of the moonpool, but it surprises me each time….), the level of the water doesn’t change!

Let’s imagine the same phenomena at a smaller scale! This is a little experiment to try at home. When you put a plastic straw in a glass, the water in your glass will rise in the straw but only until its top! The water will stop when the pressure inside the straw and at the surface of the water in your glass is the same! It’s a question of equilibrium!

It’s the same thing when you open the moonpool on the JR, but at a bigger scale!

When you open the moonpool, the water will start to enter it because it is under pressure under the ship. But as soon as the water reaches the same pressure (atmospheric pressure) that the water around the ship is at, the water will stop rising.

And don’t be afraid: no risk of sinking because the sides of the moon pool inside the ship extend up well above the waterline. Also, the moon pool doors are closed whenever the ship is moving or in rough seas…

Maybe next time we will open the moon pool a seal will come and say “hello”! 😊

Photography by Juliane Müller

 

L’appel du large

Photography by Justin Dodd

Un matin nous partons, le cerveau plein de flamme,
Le cœur gros de rancune et de désirs amers,
Et nous allons, suivant le rythme de la lame,
Berçant notre infini sur le fini des mers.

Mais les vrais voyageurs sont ceux-là seuls qui partent
Pour partir, cœurs légers, semblables aux ballons,
De leur fatalité jamais ils ne s’écartent,
Et sans savoir pourquoi, disent toujours : Allons !

Amer savoir, celui qu’on tire du voyage !
Le monde, monotone et petit, aujourd’hui,
Hier, demain, toujours, nous fait voir notre image :
Une oasis d’horreur dans un désert d’ennui !

Charles Baudelaire, Les Fleurs du Mal

 

Tracking the age of the core

Does the grey stuff in the bowl look like common mud to you? Maybe for us but definitely not for our paleontologists! This is a very special part of the core, delivered quickly to their lab soon after the core reached the core deck. These sediments were in the core catcher, at the bottom of the core. They are the oldest sediments of each core that we recover and our paleontologists come at each “core on deck” call on the catwalk to receive their special gift. They must quickly determine the age of the sample, and relay that to the science team.

Tracking the age of sediments using microfossils?

Paleontologists will determine the age of sediments by using the microfossil assemblages contained within them. In order for this approach to work, the fossils used must be widespread geographically and the sediments must contain a lot of different species.

Let’s try to do the job of one of them, Giuseppe Cortese, our radiolarian micropaleontologist onboard during Expedition 374. In this hard mud, Giuseppe will find tiny glass skeletons of radiolarians and use the species found in the core catcher to give an estimation of the age of the sediments.

But, before putting ourselves in his shoes, we have to keep in mind that species are not unchanging. They appear, evolve and disappear. Some of them evolved slowly and have existed for long time periods. Therefore, these fossils don’t provide a very good estimate of the age of the sediment. Short-lived species make our micropaleontology team happy.

Above is an example of rapid evolution within the radiolarian genus Podocyrtis in the middle Eocene (~45 million years ago). You can see the development of pores and the change in general shape between each species (Sanfilippo et al., 1985)

Giuseppe is looking for particular species which give very specific constraints on the ages. Take a look at some of the species that he found in a core catcher:

So now, it’s your time to play. By using this partial Radiolarian zonation below, you should be able to estimate an age for that core.

Need some clues?

The fact that we find the species Antarctissa cylindrica in the sediment tells us that the age of that sample is older than 0.64 Ma as this species went extinct at 0.64 Ma and therefore should not be found in sediment that is younger than that.

The presence of Helotholus vema gives is more helpful because this species only lived between 4.59 and 2.40 Ma.

The first appearance of Cyladophora davisiana is at 2.61 Ma. As we find this species in the same sediment sample as Helotholus vema, this means that we can narrow our time interval down to 2.61 to 2.40 Ma (around the end of the Pliocene to the early Pleistocene).

The first appearance of Desmospyris spongiosa is less well known (around 2.46 Ma), which is why it isn’t on the zonation chart above, but the approximate age of its evolution is coherent with our previous estimation.

Have you noticed that radiolarians are not alone in the slides? Some diatoms also hide in this sample!

Now, it’s time for David Harwood, our night shift diatom specialist, to play.

Will you be able to estimate the age of the sample using the fossil diatoms that he has found?

A few clues

Thalassiosira inura lived from 4.9 Ma to 2 Ma. David also found Thalassiosora vulnifica in this sample. This species allows us to limit the time interval of the sample to between 3.2 and 2.2 Ma.

Actinocyclus maccollumii provides an even better constraint on the age because its first appearance is at 2.8 Ma and its last appearance at 2.4 Ma, and because Actinocylcus fasciculatus first appeared (evolved) at 2.7 Ma, David can estimate a time range for this sample of 2.7 to 2.4 Ma.

So, according to Giusseppe and David, whose data agree, our core catcher sample is estimated to be 2.6-2.4 Ma, which means at the end of the Pliocene to early Pleistocene.

Why use so many species? Why is one short lived species not enough?

This is mainly because one species is not a good indicator of a former ecosystem. A single species could be reworked from older sediments?

Targeting the age of the cores is not the only skill of our paleontogists on board. They are also able to estimate former oceanic temperatures, for example, or whether the oceans were cold enough to freeze. Stay tuned if you want to know more about this topic!